---
MARKER : "2014_solar_phys_jmejia_ambriz"
TYPE   : "in_journal"
AUTHOR : "Mejia-Ambriz, J.C., Aguilar-Rodriguez, E., Jackson, B.V., Buffington, A, Gonzalez-Esparza, J.A., Tokumaru, M., Hick, P.P."
AFFIL  : "UCSD-CASS-SHPG,UNAM-MEXART,UCSD-CASS-SHPG,UCSD-CASS-SHPG,UNAM-MEXART,NAGOYA-STELAB,UCSD-CASS-SHPG"
TITLE  : "Comparison of solar wind speeds from wavelet and Fourier analysis in IPS data"
SERIAL : "Solar Phys."
VOLUME : "XXX (X)"
PAGE   : "(submitted)"
YEAR   : "2014-07"
TOPKEY : "IPS, solar wind"
ABS    : "The power spectra of intensity fluctuations in interplanetary scintillation (IPS) observations can be used to estimate solar wind speeds in the inner heliosphere. We obtain and then compare IPS spectra from both wavelet and Fourier analyses for 12 time series records of the radio source 3C48; these observations were carried out at Japan's STEL facility, at 327 MHz. We show that wavelet and Fourier analyses yield very similar power spectra. Thus, when fitting a model to the spectra to determine the solar wind speeds, both yield comparable results. Moreover, we have previously shown that these resulting speeds generally agree with those obtained by the more direct multi-station technique, a valuable certification of this means of determining solar wind speed from single-station IPS measurements. Even though spectra from wavelet and Fourier closely match each other for solar wind speed purposes, those from the wavelet analysis are slightly cleaner, which is reflected in an apparent level of intensity fluctuations that is enhanced, being ~13% higher."

---
MARKER : "2014_apj_793_54"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Yu, H.-S., Buffington, A., Hick, P.P."
TITLE  : "The dynamic character of the solar wind"
SERIAL : "Astrophys. J."
VOLUME : "793 (1)"
PAGE   : "54-60"
YEAR   : "2014-09"
DOI    : "10.1088/0004-637X/793/1/54"
TOPKEY : "Hinode, SOHO-LASCO, STEREO-COR2, polar jet, coronal hole"
ABS    : "The SOlar and Heliospheric Observatory (SOHO) Large Angle Spectroscopic COronagraph (LASCO) C2 and the Solar TErrestrial RElations Observatory (STEREO) COR2A coronagraph images, when analyzed using correlation tracking techniques, show a surprising result in places ordinarily thought of as 'quiet' solar wind above the poles in coronal hole regions. Instead of the static well-ordered flow and gradual acceleration normally expected, coronagraph images show outflow in polar coronal holes consisting of a mixture of intermittent slow and fast patches of material. We compare measurements of this highly-variable solar wind from C2 and COR2A images, and show that both coronagraphs measure essentially the same structures. Measurements of the mean velocity as a function of height of these structures are compared with mass flux determinations of the solar wind outflow in the large polar coronal hole regions and give similar results"

---
MARKER : "2014_apj_784_166"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Yu, H.-S., Jackson, B.V., Buffington, A., Hick, P.P., Shimojo, M., Sako, N."
TITLE  : "The three-dimensional analysis of Hinode polar jets using images from LASCO C2, the STEREO COR2 coronagraphs, and SMEI"
SERIAL : "Astrophys. J."
VOLUME : "784 (2)"
PAGE   : "166-174"
YEAR   : "2014-04"
DOI    : "10.1088/0004-637X/784/2/166"
TOPKEY : "Coriolis-SMEI, Hinode, SOHO-LASCO, STEREO-COR2, polar jet, coronal hole"
ABS    : "Images recorded by the X-ray Telescope (XRT) onboard the Hinode spacecraft are used to provide high cadence observations of solar jetting activity. A selection of the brightest of these polar jets shows a positive correlation with high-speed responses traced into the interplanetary medium. LASCO C2 and STEREO COR2 coronagraph images measure the coronal response to some of these largest jets, and also the nearby background solar wind velocity, thereby giving a determination of their speeds that we compare with Hinode observations. When using the full SMEI (Solar Mass Ejection Imager) data set, we track these same high speed solar jet responses into the inner heliosphere and from these analyses determine their mass, flow energies, and the extent to which they retain their identity at large solar distances."

---
MARKER : "2013_solar_phys_285_151"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Clover, J.M., Hick, P.P., Buffington, A., Bisi, M.M., Tokumaru, M."
TITLE  : "Inclusion of real-time in-situ measurements into the UCSD time-dependent tomography and its use as a forecast algorithm"
EDITOR : "Bisi, M.M., Harrison, R.A., Lugaz, N."
CTITLE : "Topical Issue: Observations and Modelling of the Inner Heliosphere"
SERIAL : "Solar Phys."
VOLUME : "285 (1-2)"
PAGE   : "151-165"
YEAR   : "2013-07"
DOI    : "10.1007/s11207-012-0102-x"
TOPKEY : "space weather"
ABS    : "The University of California, San Diego (UCSD) three-dimensional (3D) time-dependent tomography program, used for over a decade to reconstruct and forecast coronal mass ejections (CMEs), does so from observations of interplanetary scintillation (IPS) taken using the Solar-Terrestrial Environment Laboratory (STELab) radio arrays in Japan. An earlier article (Jackson et al. in Solar Phys. 265, 245, 2010) demonstrated how in-situ velocity measurements from the Advanced Composition Explorer (ACE) space-borne instrumentation can be used in addition to remote-sensing data to constrain a time-dependent tomographic velocity solution. Here we extend this in-situ inclusion to density measurements, and show how this constrains the tomographic density solution. Supplementing remote-sensing observations with in-situ measurements provides additional information to construct an iterated solar-wind parameter that is propagated outward from near the solar surface past the measurement location, and throughout the volume. As in the case of velocity when this is done, the largest changes within the volume are close to the radial directions around Earth that incorporate the in-situ measurements; the inclusion significantly reduces the uncertainty in extending these measurements to global 3D reconstructions that are distant in time and space from the spacecraft. At Earth, this analysis provides a finely tuned real-time result up to the latest time for which in-situ measurements are available, and enables more-accurate extension of these results near Earth to those remotely sensed. We show examples of this new algorithm using real-time STELab IPS data that were used in our forecasts throughout Carrington rotations 2010 through 2016, and we provide one metric prescription that we have used to determine the forecasting accuracy one, two, and three days in advance of the time data become available to analyze from STELab. We show that the accuracy is considerably better than assuming persistence of the same signal over one to two days in advance of when the data are available."

---
MARKER : "2013_solar_phys_285_317"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Webb, D.F., Mostl, C., Jackson, B.V., Bisi, M.M., Howard, T.A., Mulligan, T., Jensen, E.A., Jian, L.K., Davies, J.A., de Koning, C.A., Liu, Y., Temmer, M., Clover, J.M., Farrugia, C.J., Harrison, R.A., Nitta, N., Odstrcil, D., Tappin, S.J., Yu, H.S"
TITLE  : "Heliospheric imaging of 3D density structures during the multiple coronal mass ejections of late July to early August 2010"
EDITOR : "Bisi, M.M., Harrison, R.A., Lugaz, N."
CTITLE : "Topical Issue: Observations and Modelling of the Inner Heliosphere"
SERIAL : "Solar Phys."
VOLUME : "285 (1-2)"
PAGE   : "317-348"
YEAR   : "2013-07"
DOI    : "10.1007/s11207-013-0260-5"
TOPKEY : "Coriolis-SMEI"
ABS    : "It is usually difficult to gain a consistent global understanding of a coronal mass ejection (CME) eruption and its propagation when only near-Sun imagery and the local measurements derived from single-spacecraft observations are available. Three-dimensional (3D) density reconstructions based on heliospheric imaging allow us to 'fill in' the temporal and spatial gaps between the near-Sun and in situ data to provide a truly global picture of the propagation and interactions of the CME as it moves through the inner heliosphere. In recent years the heliospheric propagation of dense structures has been observed and measured by the heliospheric imagers of the Solar Mass Ejection Imager (SMEI) and on the twin Solar TErrestrial RElations Observatory (STEREO) spacecraft. We describe the use of several 3D reconstruction techniques based on these heliospheric imaging data sets to distinguish and track the propagation of multiple CMEs in the inner heliosphere during the very active period of solar activity in late July -- early August 2010. We employ 3D reconstruction techniques used at the University of California, San Diego (UCSD) based on a kinematic solar wind model, and also the empirical Tappin-Howard model. We compare our results with those from other studies of this active period, in particular the heliospheric simulations made with the ENLIL model by Odstrcil et al. (J. Geophys. Res., 2013) and the in situ results from multiple spacecraft provided by Mostl et al. (Astrophys. J. 758, 10-28, 2012). We find that the SMEI results in particular provide an overall context for the multiple-density flows associated with these CMEs. For the first time we are able to intercompare the 3D reconstructed densities with the timing and magnitude of in situ density structures at five spacecraft spread over 150 degrees in ecliptic longitude and from 0.4 to 1 AU in radial distance. We also model the magnetic flux-rope structures at three spacecraft using both force-free and non-force-free modelling, and compare their timing and spatial structure with the reconstructed density flows."

---
MARKER : "2013_ssr_180_1"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Howard, T.A., Bisi, M.M., Buffington, A., Clover, J.M., Cooke, M.P., Eyles, C.J., Hick, P.P., Holladay, P.E., Jackson, B.V., Johnston, J.C., Kahler, S.W., Kuchar, T.A., Mizuno, D.R., Penny, A.J., Price, S., Radick, R.R., Simnett, G.M., Tappin, S.J., Waltham, N.R., Webb, D.F."
TITLE  : "The Solar Mass Ejection Imager and its heliospheric imaging legacy"
SERIAL : "Space Sci. Rev."
VOLUME : "180"
PAGE   : "1-38"
YEAR   : "2013-06"
DOI    : "10.1007/s11214-013-9992-7"
TOPKEY : "heliospheric imaging, solar wind, solar mass ejections, corotating interaction regions, Coriolis-SMEI"
ABS    : "The Solar Mass Ejection Imager (SMEI) was the first of a new class of heliospheric and astronomical white-light imager. A heliospheric imager operates in a fashion similar to coronagraphs, in that it observes solar photospheric white light that has been Thomson scattered by free electrons in the solar wind plasma. Compared with traditional coronagraphs, this imager differs in that it observes at much larger angles from the Sun. This in turn requires a much higher sensitivity and wider dynamic range for the measured intensity. SMEI was launched on the Coriolis spacecraft in January 2003 and was deactivated in September 2011, thus operating almost continuously for nearly nine years. Its primary objective was the observation of interplanetary transients, typically coronal mass ejections (CMEs), and tracking them continuously throughout the inner heliosphere. Towards this goal it was immediately effective, observing and tracking several CMEs in the first month of mission operations, with some 400 detections to follow. Along with this primary science objective, SMEI also contributed to many and varied scientific fields, including studies of corotating interaction regions (CIRs), the high-altitude aurora, zodiacal light, Gegenschein, comet tail disconnections and motions, and variable stars. It was also able to detect and track Earth-orbiting satellites and space debris. Along with its scientific advancements, SMEI also demonstrated a significantly improved accuracy of space weather prediction, thereby establishing the feasibility and usefulness of operational heliospheric imagers. In this paper we review the scientific and operational achievements of SMEI, discuss lessons learned, and present our view of potential next steps in future heliospheric imaging."

---
MARKER : "2013_ssw13_aip_1539_364"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Buffington, A., Clover, J.M., Hick, P.P., Yu, H.-S., Bisi, M.M."
AFFIL  : "UCSD-CASS-SHPG, UNIV-ABER-IMAPS"
TITLE  : "Using comet plasma tails to study the solar wind"
EDITOR : "Zank, G.P., Borovsky, J., Bruno, R., Cirtain, J., Cranmer, S., Elliott, H., Giacalone, J., Gonzalez, W., Li, G., Marsch, E., Moebius, E., Pogorelov, N., Spann, J., Verkhoglyadova, O."
CTITLE : "Proc. Solar Wind 13"
SERIAL : "AIP. Conf. Proc."
VOLUME : "1539"
PAGE   : "364-369"
YEAR   : "2013-06"
DOI    : "10.1063/1.4811062"
TOPKEY : "Coriolis-SMEI, comet plasma tail"
PLACE  : "Big Island, HI, US (2012-06)"
ABS    : "The plasma tails of comets have been used as probes of the solar wind for many years, and well before direct solar wind measurements. Now, analyses utilizing the much greater regularity and extent of comet tails imaged from space detail outward solar wind flow much better than was previously possible. These analyses mark the location of the solar wind flow in three-dimensions over time much as do in-situ measurements. Data from comet plasma tails using coronagraphs and heliospheric white-light imagers provide a view closer to the Sun than where spacecraft have ventured to date. These views show that this flow is chaotic and highly variable, and not the benign regular outward motion of a quiescent plasma. While this is no surprise to those who study and characterize the solar wind in situ or use remotely-sensed interplanetary scintillation (IPS) techniques, these spacecraft images provide a visualization of this as never-before possible. Here we summarize the results of an analysis that determines solar wind velocity from multiple comet tails that were observed by the Solar Mass Ejection Imager (SMEI) and also by the inner Heliospheric Imager (HI) on board the Solar Terrestrial Relations Observatory Ahead (STEREOA) spacecraft. Finally, we present results using a similar analysis that measures this same behavior using coronagraph observations in the low corona."

---
MARKER : "2013_ssw13_aip_1539_90"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Yu, H.-S., Jackson, B.V., Clover, J.M., Buffington, A."
AFFIL  : "UCSD-CASS-SHPG"
TITLE  : "The analysis of polar jet responses using images from the LASCO C2 and STEREO COR 2 coronagraphs"
EDITOR : "Zank, G.P., Borovsky, J., Bruno, R., Cirtain, J., Cranmer, S., Elliott, H., Giacalone, J., Gonzalez, W., Li, G., Marsch, E., Moebius, E., Pogorelov, N., Spann, J., Verkhoglyadova, O."
CTITLE : "Proc. Solar Wind 13"
SERIAL : "AIP. Conf. Proc."
VOLUME : "1539"
PAGE   : "90-93"
YEAR   : "2013-06"
DOI    : "10.1063/1.4810997"
TOPKEY : "coronal hole, polar jet, solar wind, coronal mass ejection, Coriolis-SMEI"
PLACE  : "Big Island, HI, US (2012-06)"
ABS    : "High cadence images taken by the X-Ray Telescope (XRT) onboard Hinode and the Solar Dynamics Observatory Atmospheric Imaging Assembly (AIA) instrument provide an opportunity to observe solar jetting activity. The brightest several of these polar jets show a positive correlation with high-speed responses traced into the interplanetary medium, and have been reported in the full SMEI (Solar Mass Ejection Imager) data set images at large solar distances in the heliosphere where they retain a semblance of their original identity. LASCO C2 and STEREO COR 2 coronagraph images allow measurements of the coronal response to some of these jets, and the nearby background solar wind velocity, giving a determination of their speeds and energies that we can compare with Hinode and AIA observations. In this preliminary study we document two of these solar jet traversals into the inner heliosphere in the region intermediate to this region and the XRT and AIA observations."

---
MARKER : "2012_iac_aip_1500_147"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Yu, H.-S., Jackson, B.V., Hick, P.P., Buffington, A., Clover, J.M., Tokumaru, M."
TITLE  : "3-D reconstruction of the inner heliosphere from remote-sensing data: a global solar wind boundary that includes CME transient effects"
EDITOR : "Hu, Q., Li, G., Zank, G.P., Ao, X., Verkhoglyadova, O., Adams, J.H."
CTITLE : "11^th Int. Astrophysics Conf. on Space weather: The space radiation environment"
SERIAL : "AIP. Conf. Proc."
VOLUME : "1500"
PAGE   : "147-152"
YEAR   : "2012-11"
DOI    : "10.1063/1.4768758"
PLACE  : "Palm Springs, CA, US (2012-03)"
TOPKEY : "solar wind"
ABS    : "At UCSD, remote-sensing analyses of the inner heliosphere have been regularly carried out using interplanetary scintillation (IPS) data for almost two decades. These analyses have measured and reconstructed 3D solar wind structure throughout this time period. These global results, especially using Solar-Terrestrial Environment Laboratory (STELab) IPS observations, provide time-dependent density and velocity that is nearly complete over the whole heliosphere for the major part of each year and with a time cadence of about one day. When using the volumetric velocity from this time-dependent tomography, we can accurately convect solar surface magnetic fields outward and thus provide values of the magnetic field throughout the global volume. We can extract a 'boundary' at any height in the inner heliosphere from this analysis. These extrapolations also allow us to trace the magnetic connection of any heliospheric location back to the inner boundary surface as an approximation to the propagation path of the solar energetic particles. Here we present sample determinations of these global solar wind boundaries from recent IPS data, and provide some of the details that allow the interpolation of these boundary values across the STELab data 'outage' periods."

---
MARKER : "2012_adv_geosci_st_30_93"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Hick, P.P., Buffington, A., Clover, J.M., Tokumaru, M."
TITLE  : "Forecasting transient heliospheric solar wind parameters at the location of the inner planets"
SERIAL : "Advances in Geosciences: Solar and Terrestrial Science"
VOLUME : "30"
PAGE   : "93-115"
YEAR   : "2012-11"
DOI    : "10.1142/9789814405744_0007"
TOPKEY : "IPS, Coriolis-SMEI"
ABS    : "Remotely-sensed interplanetary scintillation (IPS) from the solar-terrestrial environment laboratory (STELab)system, and Thomson-scattering observations from the U.S. Air Force/NASA Solar Mass Ejection Imager (SMEI) allow the determination of solar wind parameters at the locations of the inner planets. We show a 3D analysis technique developed to provide daily-cadence transient solar wind forecasts of velocity and density at Earth and the inner planets. These now include in-situ measurements near Earth available in real time. Where in-situ measurements are available these real-time analyses are compared with the predicted values. Using the global velocity measurements available from IPS analysis and daily updated magnetograms from the National Solar Observatory, we are also able toproject outward solar-surfacemagnetic fields in order to provide reasonable global in-situ magnetic-field component trends from one day to the next. This paper summarizes the analysis available and current progress in using the STELab, Japan real-time data for validating these forecasts. A discussion is also provided as to how we can derive more meaningful future information from these remotely-sensed heliospheric measurements."

---
MARKER : "2012_adv_geosci_st_30_69"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V."
TITLE  : "The 3D analysis of the heliosphere using interplanetary scintillation and Thomson scattering observations"
EDITOR : "Bhardwaj, A."
SERIAL : "Advances in Geosciences: Solar and Terrestrial Science"
VOLUME : "20"
PAGE   : "69-91"
YEAR   : "2012-11"
DOI    : "10.1142/9789814405744_0006"
TOPKEY : "Coriolis-SMEI"
ABS    : "Both interplanetary scintillation (IPS) and Thomson-scattering observations from the U.S. Air Force/NASA Solar Mass Ejection Imager (SMEI) allow a determination of velocity and density in the inner heliosphere and its forecast from remote-sensing heliospheric observations. Recent solar missions, such as Hinode, STEREO, and SDO, and resultant modeling analysis using these data enhance our ability to measure detailed aspects of specific solar events, including their outflow and three-dimensional structure. Current success in this 3D heliospheric endeavor includes the analysis of heliospheric structures that are also measured in situ: interplanetary Coronal Mass Ejections (CMEs), shocks, solar co-rotating structures, and the energy transport provided by solar wind plasma throughout the heliosphere. This report highlights a portion of the work on this multi-faceted topic."

---
MARKER : "2012_lsrp_9_3"
TYPE   : "in_journal"
AUTHOR : "Webb, D.F., Howard, T.A."
TITLE  : "Coronal mass ejections: observations"
SERIAL : "Living Rev. in Solar Phys."
VOLUME : "3"
PAGE   : "(81 pages)"
YEAR   : "2012-06"
URL    : "http://www.livingreviews.org/lrsp-2012-3"
TOPKEY : "Coriolis-SMEI"
ABS    : "Solar eruptive phenomena embrace a variety of eruptions, including flares, solar energetic particles, and radio bursts. Since the vast majority of these are associated with the eruption, development, and evolution of coronal mass ejections (CMEs), we focus on CME observations in this review. CMEs are a key aspect of coronal and interplanetary dynamics. They inject large quantities of mass and magnetic flux into the heliosphere, causing major transient disturbances. CMEs can drive interplanetary shocks, a key source of solar energetic particles and are known to be the major contributor to severe space weather at the Earth. Studies over the past decade using the data sets from (among others) the SOHO, TRACE, Wind, ACE, STEREO, and SDO spacecraft, along with ground-based instruments, have improved our knowledge of the origins and development of CMEs at the Sun and how they contribute to space weather at Earth. SOHO, launched in 1995, has provided us with almost continuous coverage of the solar corona over more than a complete solar cycle, and the heliospheric imagers SMEI (2003 - 2011) and the HIs (operating since early 2007) have provided us with the capability to image and track CMEs continually across the inner heliosphere. We review some key coronal properties of CMEs, their source regions and their propagation through the solar wind. The LASCO coronagraphs routinely observe CMEs launched along the Sun-Earth line as halo-like brightenings. STEREO also permits observing Earth-directed CMEs from three different viewpoints of increasing azimuthal separation, thereby enabling the estimation of their three-dimensional properties. These are important not only for space weather prediction purposes, but also for understanding the development and internal structure of CMEs since we view their source regions on the solar disk and can measure their in-situ characteristics along their axes. Included in our discussion of the recent developments in CME-related phenomena are the latest developments from the STEREO and LASCO coronagraphs and the SMEI and HI heliospheric imagers."

---
MARKER : "2012_apj_750_45"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Harrison, R.A., Davies, J.A., Mostl, C., Liu, Y., Temmer, M., Bisi, M.M., Eastwood, J.P., de Koning, C.A., Nitta, N., Rollett, T., Farrugia, C.J., Forsyth, R.J., Jackson, B.V., Jensen, E.A., Kilpua, E.K.J., Odstrcil, D., Webb, D.F."
TITLE  : "An analysis of the origin and propagation of the multiple coronal mass ejections of 2010 August 1"
SERIAL : "Ap. J."
VOLUME : "750 (1)"
PAGE   : "45"
YEAR   : "2012-04"
DOI    : "10.1088/0004-637X/750/1/45"
TOPKEY : "Coriolis-SMEI"
ABS    : "On 2010 August 1, the northern solar hemisphere underwent significant activity that involved a complex set of active regions near central meridian with, nearby, two large prominences and other more distant active regions. This activity culminated in the eruption of four major coronal mass ejections (CMEs), effects of which were detected at Earth and other solar system bodies. Recognizing the unprecedented wealth of data from the wide range of spacecraft that were available -- providing the potential for us to explore methods for CME identification and tracking, and to assess issues regarding onset and planetary impact -- we present a comprehensive analysis of this sequence of CMEs. We show that, for three of the four major CMEs, onset is associated with prominence eruption, while the remaining CME appears to be closely associated with a flare. Using instrumentation on board the Solar Terrestrial Relations Observatory spacecraft, three of the CMEs could be tracked out to elongations beyond 50° their directions and speeds have been determined by various methods, not least to assess their potential for Earth impact. The analysis techniques that can be applied to the other CME, the first to erupt, are more limited since that CME was obscured by the subsequent, much faster event before it had propagated far from the Sun; we discuss the speculation that these two CMEs interact. The consistency of the results, derived from the wide variety of methods applied to such an extraordinarily complete data set, has allowed us to converge on robust interpretations of the CME onsets and their arrivals at 1 AU."

---
MARKER : "2012_asr_49_162"
TYPE   : "in_journal"
AUTHOR : "Mizuno, D.R., Price, S.D., Kraemer, K.E., Kuchar, T.A., Johnston, J.C."
TITLE  : "Debris swarms seen by SMEI"
SERIAL : "Adv. Space Res."
VOLUME : "49 (1)"
PAGE   : "162-176"
YEAR   : "2012-01"
DOI    : "10.1016/j.asr.2011.09.006"
TOPKEY : "Coriolis-SMEI"
ABS    : "The large 3°×60° fields-of-view of the Solar Mass Ejection Imager (SMEI) instruments are oriented on the stabilized Coriolis satellite to image most of the sky each Sun-synchronous orbit. Besides observing coronal mass ejections, the SMEI mission objective, SMEI also has detected a plethora of Earth-orbiting satellites (resident space objects or RSOs) brighter than ~8th magnitude at a rate of about 1 per minute. Occasionally, SMEI sees an RSO swarm: a sudden onset of a large number of RSOs, many more than the nominal rate, upto dozens detected in a 4-s frame. These swarms usually last for a few minutes. A sample of six such RSO ensembles is analyzed in this paper in which the distance and the direction of the velocity vector for individual objects are estimated. We present the observational evidence indicating that the swarms must be near-field objects traveling in orbits near that of Coriolis, and that the relatively speeds between the objects and Coriolis are low. Further, analyses indicate that the RSOs are quite close (<20 m) and are generally moving radially away from the satellite. The predicted encounter geometries for Coriolis passing through or near a small debris cloud is, generally, quite inconsistent with the observations. The most likely explanation consistent with the observations is that SMEI is seeing debris being ejected from the Coriolis spacecraft itself. An analysis of distance and brightness for a subset of the RSOs indicates that the median diameter of the debris particles is ~80 micrometre."

---
MARKER : "2011_celest_mech_dyn_astr_111_363"
TYPE   : "in_journal"
AUTHOR : "Fienga, A., Laskar, J., Kuchynka, P., Manche, H., Desvignes, G., Gastineau, M., Cognard, I., Theureau, G."
TITLE  : "The INPOP10a planetary ephemeris and its applications in fundamental physics"
SERIAL : "Celest. Mech. Dyn. Astr."
VOLUME : "111"
PAGE   : "363-385"
YEAR   : "2011-11"
DOI    : "10.1007/s10569-011-9377-8"
TOPKEY : "ephemeris"
ABS    : "Compared to the previous INPOP versions, the INPOP10a planetary and lunar ephemeris has several improvements. For the planets of our Solar System, no big change was brought in the dynamics but improvements were implemented in the fitting process, the data sets used in the fit and in the selection of fitted parameters. We report here the main characteristics of the planetary part of INPOP10a like the fit of the product of the solar mass with the gravitational constant (G × Msun) instead of the astronomical unit. Determinations of PPN parameters as well as adjustments of the Sun J2 and of asteroid masses are also presented. New advances of nodes and perihelia of planets were also estimated and are given here. As for INPOP08, INPOP10a provides to the user, positions and velocities of the planets, the Moon, the rotation angles of the Earth and the Moon as well as TT-TDB Chebyshev polynomials at http://www.imcce.fr/inpop."

---
MARKER : "2011_celest_mech_dyn_astr_109_101"
TYPE   : "in_journal"
AUTHOR : "Archinal, B.A., A'Hearn, M.F., Bowell, E., Conrad, A., Consolmagno, G.J., Courtin, R., Fukushima, T., Hestroffer, D., Hilton, J.L., Krasinsky, G.A., Neumann, G., Oberst, J., Seidelmann, P.K., Stooke, P., Tholen, D.J., Thomas, P.C., Williams, I.P."
TITLE  : "Report of the IAU Working Group on Cartographic Coordinates and Rotational Elements: 2009"
SERIAL : "Celest. Mech. Dyn. Astr."
VOLUME : "109"
PAGE   : "101-135"
YEAR   : "2011-11"
DOI    : "10.1007/s10569-010-9320-4"
TOPKEY : "ephemeris"
ABS    : "Every three years the IAU Working Group on Cartographic Coordinates and Rotational Elements revises tables giving the directions of the poles of rotation and the prime meridians of the planets, satellites, minor planets, and comets. This report takes into account the IAU Working Group for Planetary System Nomenclature (WGPSN) and the IAU Committee on Small Body Nomenclature (CSBN) definition of dwarf planets, introduces improved values for the pole and rotation rate of Mercury, returns the rotation rate of Jupiter to a previous value, introduces improved values for the rotation of five satellites of Saturn, and adds the equatorial radius of the Sun for comparison. It also adds or updates size and shape information for the Earth, Mars' satellites Deimos and Phobos, the four Galilean satellites of Jupiter, and 22 satellites of Saturn. Pole, rotation, and size information has been added for the asteroids (21) Lutetia, (511) Davida, and (2867) Steins. Pole and rotation information has been added for (2) Pallas and (21) Lutetia. Pole and rotation and mean radius information has been added for (1) Ceres. Pole information has been updated for (4) Vesta. The high precision realization for the pole and rotation rate of the Moon is updated. Alternative orientation models for Mars, Jupiter, and Saturn are noted. The Working Group also reaffirms that once an observable feature at a defined longitude is chosen, a longitude definition origin should not change except under unusual circumstances. It is also noted that alternative coordinate systems may exist for various (e.g. dynamical) purposes, but specific cartographic coordinate system information continues to be recommended for each body. The Working Group elaborates on its purpose, and also announces its plans to occasionally provide limited updates to its recommendations via its website, in order to address community needs for some updates more often than every 3 years. Brief recommendations are also made to the general planetary community regarding the need for controlled products, and improved or consensus rotation models for Mars, Jupiter, and Saturn."

---
MARKER : "2011_jastp_73_1317"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Hamilton, M.S., Hick, P.P., Buffington, A., Bisi, M.M., Clover, J.M., Tokumaru, M., Fujiki, K."
TITLE  : "Solar Mass Ejection Imager (SMEI) 3-D reconstruction of density enhancements behind interplanetary shocks: in-situ comparison near Earth and at STEREO"
EDITOR : "Mierla, M., Srivastava, N., Rodriguez, L."
CTITLE : "On three-dimensional aspects of CMEs, their source regions and interplanetary manifestations (special issue)"
SERIAL : "J. Atmospheric and Solar-Terrestrial Physics"
VOLUME : "73 (11-12)"
PAGE   : "1317-1329"
YEAR   : "2011-07"
DOI    : "10.1016/j.jastp.2010.11.023"
TOPKEY : "Coriolis-SMEI, interplanetary shocks"
ABS    : "SMEI and IPS remotely observe increased brightness and velocity enhancements behind interplanetary shocks that are also seen in situ. We use the UCSD time-dependent 3-D reconstruction technique to map these enhancements, and compare them with measurements at the SOHO, Wind, ACE, and STEREO spacecraft. The analyses of these shocks from hour-averaged in-situ data show that the enhanced density column associated with the shock response varies considerably between different instruments, even for in-situ instruments located at L1 near Earth. The relatively-low-resolution SMEI 3-D reconstructions generally show density enhancements, and within errors, the column excesses match those observed in situ. In these SMEI 3-D reconstructions from remotely-sensed data, the shock density enhancements appear not as continuous broad fronts, but as segmented structures. This may provide part of the explanation for the observed discrepancies between the various in-situ measurements at Earth and STEREO, but not between individual instruments near L1."

---
MARKER : "2011_jastp_73_1214"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Hick, P.P., Buffington, A., Bisi, M.M., Clover, J.M., Tokumaru, M., Kojima, M., Fujiki, K."
TITLE  : "Three-dimensional reconstruction of heliospheric structure using iterative tomography: a review"
EDITOR : "Mierla, M., Srivastava, N., Rodriguez, L."
CTITLE : "On three-dimensional aspects of CMEs, their source regions and interplanetary manifestations (special issue)"
SERIAL : "J. Atmospheric and Solar-Terrestrial Physics"
VOLUME : "73 (10)"
PAGE   : "1214-1227"
YEAR   : "2011-06"
DOI    : "10.1016/j.jastp.2010.10.007"
TOPKEY : "Coriolis-SMEI, IPS"
ABS    : "Current perspective and in-situ analyses using data from NASA's twin Solar TErrestrial RElations Observatory (STEREO) spacecraft have focused studies on ways to provide three-dimensional (3-D) reconstructions of coronal and heliospheric structure. Data from STEREO are proceeded by and contemporaneous with many other types of data and analysis techniques; most of the latter have provided 3-D information by relying on remote-sensing information beyond those of the near corona (outside 10 RS). These include combinations of past data from the Helios spacecraft and the Solwind coronagraphs and, continuing from the past to the present, from observations of interplanetary scintillation (IPS) and the Solar Mass Ejection Imager (SMEI) instrument. In this article we review past and ongoing analyses that have led to a current great wealth of 3-D information. When properly utilized, these analyses can provide not only shapes of CME/ICMEs but also a characterization of any solar wind structure or global outflow."

---
MARKER : "2011_jgr_117_a05103"
TYPE   : "in_journal"
AUTHOR : "Tappin, S.J., Howard, T.A., Hampson, M.M., Thompson, R.N., Burns, C.E."
TITLE  : "On the autonomous detection of coronal mass ejections in heliospheric imager data"
SERIAL : "J. Geophys. Res."
VOLUME : "117"
PAGE   : "A05103"
YEAR   : "2011-05"
DOI    : "10.1029/2011JA017439"
TOPKEY : "Coriolis-SMEI"
ABS    : "We report on the development of an Automatic Coronal Mass Ejection (CME) Detection tool (AICMED) for the Solar Mass Ejection Imager (SMEI). CMEs observed with heliospheric imagers are much more difficult to detect than those observed by coronagraphs as they have a lower contrast compared with the background light, have a larger range of intensity variation and are easily confused with other transient activity. CMEs appear in SMEI images as very faint often-fragmented arcs amongst a much brighter and often variable background. AICMED operates along the same lines as Computer Aided CME Tracking (CACTus), using the Hough Transform on elongation-time J-maps to extract straight lines from the data set. We compare AICMED results with manually measured CMEs on almost three years of data from early in SMEI operations. AICMED identified 83 verifiable events. Of these 46 could be matched with manually identified events, the majority of the non-detections can be explained. The remaining 37 AICMED events were newly discovered CMEs. The proportion of false identification was high, at 71% of the autonomously detected events. We find that AICMED is very effective as a region of interest highlighter, and is a promising first step in autonomous heliospheric imager CME detection, but the SMEI data are too noisy for the tool to be completely automated."

---
MARKER : "2011_apj_728_31"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Li, J., Jewitt, D., Clover, J.M., Jackson, B.V."
TITLE  : "Outburst of Comet 17P/Holmes observed with the Solar Mass Ejection Imager"
SERIAL : "Astrophys. J."
VOLUME : "728 (1)"
PAGE   : "31-39"
YEAR   : "2011-02"
DOI    : "10.1088/0004-637X/728/1/31"
TOPKEY : "Coriolis-SMEI"
ABS    : "We present time-resolved photometric observations of the Jupiter family comet 17P/Holmes during its dramatic 2007 outburst. The observations, from the orbiting Solar Mass Ejection Imager (SMEI), provide the most complete measure of the whole-coma brightness, free from the effects of instrumental saturation and with a time resolution well matched to the rapid brightening of the comet. The light curve is divided into two distinct parts. A rapid rise between the first SMEI observation on UT 2007 October 24 06h 37m (mid-integration) and UT 2007 October 25 is followed by a slow decline until the last SMEI observation on UT 2008 April 6 22h 16m (mid-integration). We find that the rate of change of the brightness is reasonably well described by a Gaussian function having a central time of UT 2007 October 24.54 ± 0.01 and a full width at half-maximum of 0.44 ± 0.02 days. The maximum rate of brightening occurs some 1.2 days after the onset of activity. At the peak, the scattering cross-section grows at 10^70 ± 40 km^2 s^-1 while the (model-dependent) mass loss rates inferred from the light curve reach a maximum at 3 × 10^5 kg s^-1. The integrated mass in the coma lies in the range (2-90) × 10^10 kg, corresponding to 0.2%-10% of the nucleus mass, while the kinetic energy of the ejecta is (0.7-30) megatonnes TNT. The particulate coma mass could be contained within a shell on the nucleus of thickness 1-60 m. This is also the approximate distance traveled by conducted heat in the century since the previous outburst of 17P/Holmes. This coincidence is consistent with, but does not prove, the idea that the outburst was triggered by the action of conducted heat, possibly through the crystallization of buried amorphous ice."

---
MARKER : "2010_solar_phys_267_235"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Sixty years in solar physics"
SERIAL : "Solar Phys."
VOLUME : "267 (2)"
PAGE   : "235-250"
YEAR   : "2010-12"
DOI    : "10.1007/s11207-010-9675-4"
TOPKEY : "solar physics"
ABS    : "I recount my career in solar physics beginning at Ondrejov Observatory in 1948 and ending with my ~30 year stay at the Laboratory of Space Research in Utrecht."

---
MARKER : "2010_apj_724_829"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Buffington, A., Hick, P.P., Clover, J.M., Bisi, M.M., Webb, D."
TITLE  : "SMEI 3D reconstruction of a coronal mass ejection interacting with a corotating solar wind density enhancement: the 2008 April 26 CME"
SERIAL : "Astrophys. J."
VOLUME : "724 (2)"
PAGE   : "829-834"
YEAR   : "2010-12"
DOI    : "10.1088/0004-637X/724/2/829"
TOPKEY : "Coriolis-SMEI, solar mass ejection, corotating interaction regions"
ABS    : "The Solar Mass Ejection Imager (SMEI) has recorded the brightness responses of hundreds of interplanetary coronal mass ejections (CMEs) in the interplanetary medium. Using a three-dimensional (3D) reconstruction technique that derives its perspective views from outward-flowing solar wind, analysis of SMEI data has revealed the shapes, extents, and masses of CMEs. Here, for the first time, and using SMEI data, we report on the 3D reconstruction of a CME that intersects a corotating region marked by a curved density enhancement in the ecliptic. Both the CME and the corotating region are reconstructed and demonstrate that the CME disrupts the otherwise regular density pattern of the corotating material. Most of the dense CME material passes north of the ecliptic and east of the Sun-Earth line: thus, in situ measurements in the ecliptic near Earth and at the Solar-TErrestrial RElations Observatory Behind spacecraft show the CME as a minor density increase in the solar wind. The mass of the dense portion of the CME is consistent with that measured by the Large Angle Spectrometric Coronagraph on board the Solar and Heliospheric Observatory spacecraft, and is comparable to the masses of many other three-dimensionally reconstructed solar wind features at 1 AU observed in SMEI 3D reconstructions."

---
MARKER : "2010_apj_724_480"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Hounsell, R., Bode, M.F., Hick, P.P., Buffington, A., Jackson, B.V., Clover, J.M., Shafter, A.W., Darnley, M.J., Mawson, N.R., Steele, I.A., Evans, A., Eyres, S.P.S., O'Brien, T.J."
TITLE  : "Exquisite nova light curves from the Solar Mass Ejection Imager (SMEI)"
SERIAL : "Astrophys. J."
VOLUME : "724 (1)"
PAGE   : "480-486"
YEAR   : "2010-11"
DOI    : "10.1088/0004-637X/724/1/480"
URL    : "http://arxiv.org/abs/1009.1737"
TOPKEY : "novae, Coriolis-SMEI"
ABS    : "We present light curves of three classical novae (CNe; KT Eridani, V598 Puppis, V1280 Scorpii) and one recurrent nova (RS Ophiuchi) derived from data obtained by the Solar Mass Ejection Imager (SMEI) on board the Coriolis satellite. SMEI provides near complete skymap coverage with precision visible-light photometry at 102 minute cadence. The light curves derived from these skymaps offer unprecedented temporal resolution around, and especially before, maximum light, a phase of the eruption normally not covered by ground-based observations. They allow us to explore fundamental parameters of individual objects including the epoch of the initial explosion, the reality and duration of any pre-maximum halt (found in all three fast novae in our sample), the presence of secondary maxima, speed of decline of the initial light curve, plus precise timing of the onset of dust formation (in V1280 Sco) leading to estimation of the bolometric luminosity, white dwarf mass, and object distance. For KT Eri, Liverpool Telescope SkyCamT data confirm important features of the SMEI light curve and overall our results add weight to the proposed similarities of this object to recurrent rather than to CNe. In RS Oph, comparison with hard X-ray data from the 2006 outburst implies that the onset of the outburst coincides with extensive high-velocity mass loss. It is also noted that two of the four novae we have detected (V598 Pup and KT Eri) were only discovered by ground-based observers weeks or months after maximum light, yet these novae reached peak magnitudes of 3.46 and 5.42, respectively. This emphasizes the fact that many bright novae per year are still overlooked, particularly those of the very fast speed class. Coupled with its ability to observe novae in detail even when relatively close to the Sun in the sky, we estimate that as many as five novae per year may be detectable by SMEI."

---
MARKER : "2010_highlights_of_astronomy_15_471"
TYPE   : "in_proceedings"
AUTHOR : "Webb, D.F., Gibson, S.E., Thompson, B.J."
TITLE  : "Whole Heliosphere Interval: Overview of JD16"
EDITOR : "Corbett, I.F."
CTITLE : "IHY Global Campaign−Whole Heliosphere Interval (XXVIIth IAU General Assembly 2009)"
SERIAL : "Highlights of Astronomy"
VOLUME : "15"
PAGE   : "471-478"
YEAR   : "2010-10"
DOI    : "10.1017/S174392131001032X"
TOPKEY : "Coriolis-SMEI"
ABS    : "The Whole Heliosphere Interval is an international observing and modeling effort to characterize the three-dimensional interconnected solar-heliospheric-planetary system, i.e., the 'heliophysical' system. WHI was part of the International Heliophysical Year, on the 50th anniversary of the International Geophysical Year, and benefited from hundreds of observatories and instruments participating in IHY activities. WHI describes the 3-D heliosphere originating from solar Carrington Rotation 2068, March 20 - April 16, 2008. The focus of IAU JD16 was on analyses of observations obtained during WHI, and simulations and modeling involving those data and that period. Consideration of the WHI interval in the context of surrounding solar rotations and/or compared to last solar minimum was also encouraged. Our goal was to identify connections and commonalities between the various regions of the heliosphere."

---
MARKER : "2010_highlights_of_astronomy_15_480"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Bisi, M.M., Jackson, B.V., Clover, J.M., Hick, P.P., Buffington, A.,Tokumaru, M."
TITLE  : "A summary of 3D reconstructions of the Whole Heliosphere Interval and comparison with in-ecliptic solar wind measurements from STEREO, ACE, and Wind instrumentation"
EDITOR : "Corbett, I.F."
CTITLE : "IHY Global Campaign−Whole Heliosphere Interval (XXVIIth IAU General Assembly 2009)"
SERIAL : "Highlights of Astronomy"
VOLUME : "15"
PAGE   : "480-483"
YEAR   : "2010-10"
DOI    : "10.1017/S1743921310010331"
TOPKEY : "IPS"
ABS    : "We present a summary of results from simultaneous Solar-Terrestrial Environment Laboratory (STELab) Interplanetary Scintillation (IPS), STEREO, ACE, and Wind observations using three-dimensional reconstructions of the Whole Heliosphere Interval -- Carrington rotation 2068. This is part of the world-wide IPS community's International Heliosphysical Year (IHY) collaboration. We show the global structure of the inner heliosphere and how our 3-D reconstructions compare with in-ecliptic spacecraft measurements."

---
MARKER : "2010_solar_phys_265_49"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Bisi, M.M., Breen, A.R., Jackson, B.V., Fallows, R.A., Walsh, A.P., Mikic, Z., Riley, P., Owen, C.J., Gonzalez-Esparza, A., Aguilar-Rodriguez, E., Morgan, H., Jensen, E.A., Wood, A.G., Tokumaru, M., Manoharan, P.K., Chashei, I.V., Giunta, A.S., Linker, J.A., Shishov, V.I., Tyul'bashev, S.A., Agalya, G., Glubokova, S.K., Hamilton, M.S., Fujiki, K., Hick, P.P., Clover, J.M., Pinter, B."
TITLE  : "From the Sun to the Earth: the 13 May 2005 coronal mass ejection"
SERIAL : "Solar Phys."
VOLUME : "265 (1/2)"
PAGE   : "49-127"
YEAR   : "2010-08"
DOI    : "10.1007/s11207-010-9602-8"
TOPKEY : "coronal mass ejections"
ABS    : "We report the results of a multi-instrument, multi-technique, coordinated study of the solar eruptive event of 13 May 2005. We discuss the resultant Earth-directed (halo) coronal mass ejection (CME), and the effects on the terrestrial space environment and upper Earth atmosphere. The interplanetary CME (ICME) impacted the Earth's magnetosphere and caused the most-intense geomagnetic storm of 2005 with a Disturbed Storm Time (Dst) index reaching -263 nT at its peak. The terrestrial environment responded to the storm on a global scale. We have combined observations and measurements from coronal and interplanetary remote-sensing instruments, interplanetary and near-Earth in-situ measurements, remote-sensing observations and in-situ measurements of the terrestrial magnetosphere and ionosphere, along with coronal and heliospheric modelling. These analyses are used to trace the origin, development, propagation, terrestrial impact, and subsequent consequences of this event to obtain the most comprehensive view of a geo-effective solar eruption to date. This particular event is also part of a NASA-sponsored Living With a Star (LWS) study and an on-going US NSF-sponsored Solar, Heliospheric, and INterplanetary Environment (SHINE) community investigation."

---
MARKER : "2010_space_res_today_178_10"
TYPE   : "in_journal"
AUTHOR : "Webb, D.F., Biesecker, D.A., Gopalswamy, N., St. Cyr, O.C., Davila, J.M., Thompson, B.J., Simunac, K.D.C., Johnston, J.C."
TITLE  : "Using STEREO-B as an L5 space weather pathfinder mission"
SERIAL : "Space Weather Today"
VOLUME : "178"
PAGE   : "10-16"
YEAR   : "2010-08"
DOI    : "10.1016/j.srt.2010.07.004"
TOPKEY : "space weather, Coriolis-SMEI"

---
MARKER : "2010_solar_phys_265_159"
TYPE   : "in_journal"
AUTHOR : "Tappin, S.J., Howard, T.A."
TITLE  : "Reconstructing CME structures from IPS observations using a phenomenological model"
SERIAL : "Solar Phys."
VOLUME : "265 (1/2)"
PAGE   : "159-186"
YEAR   : "2010-08"
DOI    : "10.1007/s11207-010-9588-2"
TOPKEY : "IPS"
ABS    : "We present an extension of the Tappin-Howard (TH) phenomenological model (Tappin and Howard, Space Sci. Rev. 147, 55, 2009) for coronal mass ejection reconstruction to use interplanetary scintillation g-map data. The necessary changes to the model are discussed. We then use the modified model to reconstruct two major interplanetary disturbances observed using the Cambridge 3.6 ha Array in September 1980. We find that despite the lower cadence of IPS observations compared with white-light imagers, a consistent reconstruction can be generated which is in agreement with in-situ measurements and solar observations."

---
MARKER : "2010_solar_phys_265_293"
TYPE   : "in_journal"
AUTHOR : "Oberoi, D., Benkevitch, L."
TITLE  : "Remote sensing of the heliosphere with the Murchison Widefield Array"
SERIAL : "Solar Phys"
VOLUME : "265 (1/2)"
PAGE   : "293-307"
YEAR   : "2010-08"
DOI    : "10.1007/s11207-010-9580-x"
TOPKEY : "IPS"
ABS    : "The Murchison Widefield Array (MWA) is one of the new technology low frequency radio interferometers currently under construction at an extremely radio-quiet location in Western Australia. The MWA design brings to bear the recent availability of powerful high-speed computational and digital signal processing capabilities on the problem of low frequency high-fidelity imaging with a rapid cadence and high spectral resolution. Solar and heliosphere science are among the key science objectives of the MWA and have guided the array design from its very conception. We present here a brief overview of the design and capabilities of the MWA with emphasis on its suitability for solar physics and remote-sensing of the heliosphere. We discuss the solar imaging and interplanetary scintillation (IPS) science capabilities of the MWA and also describe a new software framework. This software, referred to as Haystack InterPlanetary Software System (HIPSS), aims to provide a common data repository, interface, and analysis tools for IPS data from all observatories across the world."

---
MARKER : "2010_solar_phys_265_233"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Bisi, M.M., Jackson, B.V., Breen, A.R., Dorrian, G.D., Fallows, R.A., Clover, J.M., Hick, P.P."
TITLE  : "Three-dimensional (3-D) reconstructions of EISCAT IPS velocity data in the declining phase of solar cycle 23"
SERIAL : "Solar Phys."
VOLUME : "265 (1/2)"
PAGE   : "233-244"
YEAR   : "2010-07"
DOI    : "10.1007/s11207-010-9594-4"
TOPKEY : "IPS, corotating interaction regions"
ABS    : "The European Incoherent SCATter (EISCAT) radar has been used for remote-sensing observations of interplanetary scintillation (IPS) for a quarter of a century. During the April/May 2007 observing campaign, a large number of observations of IPS using EISCAT took place to give a reasonable spatial and temporal coverage of solar wind velocity structure throughout this time during the declining phase of Solar Cycle 23. Many co-rotating and transient features were observed during this period. Using the University of California, San Diego three-dimensional (3-D) time-dependent computer assisted tomography (C.A.T.) solar-wind reconstruction analysis, we show the velocity structure of the inner heliosphere in three dimensions throughout the time interval of 20 April through 20 May 2007. We also compare to white-light remote-sensing observations of an interplanetary coronal mass ejection (ICME) seen by the STEREO Ahead spacecraft inner Heliospheric Imager on 16 May 2007, as well as to in-situ solar-wind measurements taken with near-Earth spacebourne instrumentation throughout this interval. The reconstructions show clear co-rotating regions during this period, and the time-series extraction at spacecraft locations compares well with measurements made by the STEREO, Wind, and ACE spacecraft. This is the first time such clear structures have been revealed using this 3-D technique with EISCAT IPS data as input."

---
MARKER : "2010_space_weather_8_s07004"
TYPE   : "in_journal"
AUTHOR : "Howard, T.A., Tappin, S.J."
TITLE  : "Application of a new phenomenological coronal mass ejection model to space weather forecasting"
SERIAL : "Space Weather"
VOLUME : "8"
PAGE   : "s07004"
YEAR   : "2010-07"
DOI    : "10.1029/2009SW000531"
TOPKEY : "Coriolis-SMEI"
ABS    : "Recent work by the authors has produced a new phenomenological model for coronal mass ejections (CMEs). This model, called the Tappin-Howard (TH) Model, takes advantage of the breakdown of geometrical linearity when CMEs are observed by white-light imagers at large distances from the Sun. The model extracts 3-D structure and kinematic information on the CME using heliospheric image data. This can estimate arrival times of the CME at 1 AU and impact likelihood with the Earth. Hence the model can be used for space weather forecasting. We present a preliminary evaluation of this potential with three mock trial forecasts performed using the TH Model. These are already-studied events from 2003, 2004 and 2007 but we performed the trials assuming that they were observed for the first time. The earliest prediction was made 17 hours before impact and predicted arrival times reached differences within one hour for at least one forecast for all three events. The most accurate predicted arrival time was 15 min from the actual, and all three events reach accuracies of the order of 30 min. Arrival speeds were predicted to be very similar to the bulk plasma speed within the CME near 1 AU for each event, with the largest difference around 300 km/s and the least 40 km/s. The model showed great potential and we aspire to fully validate it for integration with existing tools for space weather forecasting."

---
MARKER : "2010_solar_phys_264_433"
TYPE   : "in_journal"
AUTHOR : "Bewsher, D., Brown, D.S., Eyles, C.J., Kellett, B.J., White, G.J., Swinyard, B."
TITLE  : "Determination of the photometric calibration and large-scale flatfield of the STEREO heliospheric imagers: I. HI-1"
SERIAL : "Solar Phys."
VOLUME : "264"
PAGE   : "433-460"
YEAR   : "2010-07"
DOI    : "10.1007/s11207-010-9582-8"
TOPKEY : "heliospheric imaging"
ABS    : "The aim of this paper is to calculate an accurate large-scale flatfield for the STEREO HI-1 instruments. This is done by analysing the variation in intensity of stars in the background starfield as they pass across the CCD. In order to use the background starfield, a photometric calibration is performed which defines a HI magnitude scale and a conversion between this scale and measured intensity. The photometric calibration uses stellar spectra folded through the instrument response to make initial intensity predictions. However, a secondary prediction method based on the photometric calibration, which blends the R-, V- and B-magnitudes of a star, is derived for stars with no spectral information. To perform this calibration, an initial analysis of the shape of the point spread function was required. This indicated that the PSF for the HI-1s is well approximated by a Gaussian function and does not vary substantially from the centre of the field-of-view to the corners and is essentially constant over time.

In addition, a solar spectrum folded through the instrument response is used to determine conversion factors to convert from HI intensity units into mean solar brightness, S10 and SI units, for diffuse or extended sources."

---
MARKER : "2010_solar_phys_265_257"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Buffington, A., Hick, P.P., Bisi, M.M., Clover, J.M."
TITLE  : "A heliospheric imager for deep space: lessons learned from Helios, SMEI, and STEREO"
SERIAL : "Solar Phys."
VOLUME : "265 (1/2)"
PAGE   : "257-275"
YEAR   : "2010-06"
DOI    : "10.1007/s11207-010-9579-3"
TOPKEY : "Coriolis-SMEI"
ABS    : "The zodiacal-light photometers on the twin Helios spacecraft, the Solar Mass Ejection Imager (SMEI) on the Coriolis spacecraft, and the Heliospheric Imagers (HIs) on the Solar-TErrestrial RElations Observatory (STEREO) twin spacecraft all point the way to optimizing future remote-sensing Thomson-scattering observations from deep space. Such data could be provided by wide-angle viewing instruments on Solar Orbiter, Solar Probe, or other deep-space probes. Here, we present instrument specifications required for a successful heliospheric imager, and the measurements and data-processing steps that make the best use of this remote-sensing system. When this type of instrument is properly designed and calibrated, its data are capable of determining zodiacal-dust properties, and of three-dimensional reconstructions of heliospheric electron density over large volumes of the inner heliosphere. Such systems can measure fundamental properties of the inner heliospheric plasma, provide context for the in-situ monitors on board spacecraft, and enable physics-based analyses of this important segment of the Sun-spacecraft connection."

---
MARKER : "2010_apjl_715_l104"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Bisi, M.M., Jackson, B.V., Hick, P.P., Buffington, A., Clover, J.M., Tokumaru, M., Fujiki, K."
TITLE  : "Three-dimensional reconstructions and mass determination of the 2008 June 2 LASCO coronal mass ejection using STELab IPS observations"
SERIAL : "Astrophys. J. Lett."
VOLUME : "715 (2)"
PAGE   : "L104-L108"
YEAR   : "2010-06"
DOI    : "10.1088/2041-8205/715/2/L104"
TOPKEY : "IPS"
ABS    : "We examine and reconstruct the interplanetary coronal mass ejection (ICME) first seen in space-based coronagraph white-light difference images on 2008 June 1 and 2. We use observations of interplanetary scintillation (IPS) taken with the Solar-Terrestrial Environment Laboratory (STELab), Japan, in our three-dimensional (3D) tomographic reconstruction of density and velocity. The coronal mass ejection (CME) was first observed by the LASCO C3 instrument at around 04:17 UT on 2008 June 2. Its motion subsequently moved across the C3 field of view with a plane-of-the-sky velocity of 192 km s^-1. The 3D reconstructed ICME is consistent with the trajectory and extent of the CME measurements taken from the CDAW CME catalog. However, excess mass estimates vary by an order of magnitude from Solar and Heliospheric Observatory and Solar Terrestrial Relations Observatory coronagraphs to our 3D IPS reconstructions of the inner heliosphere. We discuss the discrepancies and give possible explanations for these differences as well as give an outline for future studies."

---
MARKER : "2010_solar_phys_265_31"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jensen, E.A., Hick, P.P., Bisi, M.M., Jackson, B.V., Clover, J.M., T. Mulligan, T."
TITLE  : "Faraday rotation response to coronal mass ejection structure"
SERIAL : "Solar Phys."
VOLUME : "265 (1/2)"
PAGE   : "31-48"
YEAR   : "2010-05"
DOI    : "10.1007/s11207-010-9543-2"
TOPKEY : "Faraday rotation, coronal mass ejections"
ABS    : "We present the results from modeling the coronal mass ejection (CME) properties that have an effect on the Faraday rotation (FR) signatures that may be measured with an imaging radio antenna array such as the Murchison Widefield Array (MWA). These include the magnetic flux rope orientation, handedness, magnetic-field magnitude, velocity, radius, expansion rate, electron density, and the presence of a shock/sheath region. We find that simultaneous multiple radio source observations (FR imaging) can be used to uniquely determine the orientation of the magnetic field in a CME, increase the advance warning time on the geoeffectiveness of a CME by an order of magnitude from the warning time possible from in-situ observations at L 1, and investigate the extent and structure of the shock/sheath region at the leading edge of fast CMEs. The magnetic field of the heliosphere is largely 'invisible' with only a fraction of the interplanetary magnetic-field lines convecting past the Earth; remote sensing the heliospheric magnetic field through FR imaging from the MWA will advance solar physics investigations into CME evolution and dynamics."

---
MARKER : "2010_adv_geosci_st_21_339"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Hick, P.P., Buffington, A., Bisi, M.M., Clover, J.M., Tokumaru, M."
TITLE  : "Solar Mass Ejection Imager (SMEI) and interplanetary scintillation (IPS) 3D-reconstructions of the inner heliosphere"
EDITOR : "Duldig, M."
CTITLE : "Proc. AOGS 2009"
SERIAL : "Advances in Geosciences: Solar and Terrestrial Science"
VOLUME : "21"
PAGE   : "339-366"
YEAR   : "2010-04"
PUBLISH: "World Scientific Publ. Co"
DOI    : "10.1142/9789812838209_0025"
TOPKEY : "Coriolis-SMEI, IPS"
ABS    : "The Solar Mass Ejection Imager (SMEI) direct white-light data as well as higher-level data products are available on our UCSD Website at http://smei.ucsd.edu/ from first light in early February 2003 to nearly the present day. These analyses provide densities in the inner heliosphere, show many familiar CMEs in three dimensions (3D) during this interval, and provide animations and individual images of them. This 3D analysis is enhanced by use of interplanetary scintillation (IPS) velocity observations to help provide the overall form of the structures reconstructed. Our time-dependent 3D reconstruction technique is discussed, and the different ways we test and validate these 3D results. These checks include both internal consistency checks, and comparisons with in situ measurements at various near-Earth spacecraft, at Ulysses, at the STEREO spacecraft, and from magnetic field data at Mars."

---
MARKER : "2010_adv_geosci_st_21_33"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Bisi, M.M., Jackson, B.V., Fallows, R.A., Dorrian, G.D., Manoharan, P.K., Clover, J.M., Hick, P.P., Buffington, A., Breen, A.R., Tokumaru, M."
TITLE  : "Solar wind and CME studies of the inner heliosphere using IPS data from STELab, ORT, and EISCAT"
EDITOR : "Duldig, M."
CTITLE : "Proc. AOGS 2008"
SERIAL : "Advances in Geosciences: Solar and Terrestrial Science"
VOLUME : "21"
PAGE   : "33-49"
YEAR   : "2010-04"
PUBLISH: "World Scientific Publ. Co"
DOI    : "10.1142/9789812838209_0003"
TOPKEY : "IPS"
ABS    : "Interplanetary scintillation (IPS) observations provide views of the solar wind at all heliographic latitudes from near 1 A.U. down to fields of view covered by coronagraphs. These observations can be used to study the propagation of the solar wind and solar transients out into interplanetary space, and also measure the inner-heliospheric response to co-rotating solar structures and coronal mass ejections (CMEs). We use a three dimensional (3D) reconstruction technique that obtains perspective views from solar co-rotating plasma and outward-flowing solar wind as observed from the Earth by iteratively fitting a kinematic solar wind model to IPS data from various observing systems. Here we use the model with both Solar Terrestrial Environment Laboratory (STELab), Japan, and Ootacamund (Ooty) Radio Telescope (ORT), India, IPS observations. This 3D modeling technique permits reconstructions of the density and velocity structures of CMEs and other interplanetary transients at a relatively coarse resolution for STELab and better for Ooty; and is dependent upon the number of observations. We present 3D reconstructions of CME events around 4-8 November 2004 from Ooty IPS observations and some preliminary reconstructions of STELab IPS observations around the Whole Heliospheric Interval (WHI). We also present some preliminary results of a CME observation by both the European Incoherent SCATter (EISCAT) radar IPS observations and those made by the Solar TErrestrial RElations Observatory (STEREO) of a CME in May 2007."

---
MARKER : "2010_apj_713_394"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Clover, J.M., Jackson, B.V., Buffington, A., Hick, P.P., Bisi, M.M."
TITLE  : "Solar wind speed inferred from cometary plasma tails using observations from Stereo HI-1"
TYPE   : "in_journal"
SERIAL : "Astrophys. J."
VOLUME : "713 (1)"
PAGE   : "394-397"
YEAR   : "2010-04"
DOI    : "10.1088/0004-637X/713/1/394"
TOPKEY : "comet plasma tail"
ABS    : "The high temporal and spatial resolution of heliospheric white-light imagers enables us to measure the propagation of plasma tails of bright comets as they travel through the interplanetary medium. Plasma tails of comets have been recognized for many years as natural probes of the solar wind. Using a new technique developed at the University of California, San Diego to measure the radial motion of the plasma tails, we measure the ambient solar wind speed, for the first time in situ at comets 2P/Encke and 96P/Machholz. We determine the enhanced solar wind speeds during an interplanetary coronal mass ejection encounter with 2P/Encke and compare these to previously modeled values, and also present solar wind speeds covering a range of latitudes for 96P/Machholz. We here apply this technique using images from the Sun-Earth Connection Coronal and Heliospheric Investigation Heliospheric Imagers (HI-1) on board the Solar TErrestrial RElations Observatory-Ahead spacecraft."

---
MARKER : "2010_solar_phys_265_245"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Hick, P.P., Bisi, M.M., Clover, J.M., Buffington, A."
TITLE  : "Inclusion of in-situ velocity measurements into the UCSD time-dependent tomography to constrain and better-forecast remote-sensing observations "
SERIAL : "Solar Phys."
VOLUME : "265 (1/2)"
PAGE   : "245-256"
YEAR   : "2010-03"
DOI    : "10.1007/s11207-010-9529-0"
TOPKEY : "Coriolis-SMEI, IPS,space weather"
ABS    : "The University of California, San Diego (UCSD) three-dimensional (3-D) time-dependent tomography program has been used successfully for a decade to reconstruct and forecast coronal mass ejections from interplanetary scintillation observations. More recently, we have extended this tomography technique to use remote-sensing data from the Solar Mass Ejection Imager (SMEI) on board the Coriolis spacecraft; from the Ootacamund (Ooty) radio telescope in India; and from the European Incoherent SCATter (EISCAT) radar telescopes in northern Scandinavia. Finally, we intend these analyses to be used with observations from the Murchison Widefield Array (MWA), or the LOw Frequency ARray (LOFAR) now being developed respectively in Australia and Europe. In this article we demonstrate how in-situ velocity measurements from the Advanced Composition Explorer (ACE) space-borne instrumentation can be used in addition to remote-sensing data to constrain the time-dependent tomographic solution. Supplementing the remote-sensing observations with in-situ measurements provides additional information to construct an iterated solar-wind parameter that is propagated outward from near the solar surface past the measurement location, and throughout the volume. While the largest changes within the volume are close to the radial directions that incorporate the in-situ measurements, their inclusion significantly reduces the uncertainty in extending these measurements to global 3-D reconstructions that are distant in time and space from the spacecraft. At Earth, this can provide a finely-tuned real-time measurement up to the latest time for which in-situ measurements are available, and enables more-accurate forecasting beyond this than remote-sensing observations alone allow."

---
MARKER : "2010_sw12_aip_1216_659"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Hick, P.P., Buffington, A., Bisi, M.M., Clover, J.M., Hamilton, M.S., Tokumaru, M., Fujiki, K."
TITLE  : "3D reconstruction of density enhancements behind interplanetary shocks from Solar Mass Ejection Imager white-light observations"
EDITOR : "Maksimovic, M., Issautier, K., Meyer-Vernet, N., Moncuquet, M., Pantellini, F."
CTITLE : "Solar Wind Twelve"
SERIAL : "AIP Conf. Proc."
VOLUME : "1216"
PAGE   : "659-662"
YEAR   : "2010-03"
DOI    : "10.1063/1.3395953"
TOPKEY : "Coriolis-SMEI, interplanetary shocks"
ABS    : "The Solar Mass Ejection Imager (SMEI) observes the increased brightness from the density enhancements behind interplanetary shocks that are also observed in situ near the Earth. We use the University of California, San Diego (UCSD) time-dependent three-dimensional (3D) reconstruction technique to map the extents of these density enhancements. Here, we examine shock-density enhancements associated with several well-known interplanetary coronal mass ejections (ICMEs) including those on 30 May 2003 and on 21 January 2005. We compare these densities with reconstructed velocities from the Solar-Terrestrial Environment Laboratory (STELab) interplanetary scintillation (IPS) observations for the 30 May 2003 ICME, and show the shock is present at the front edge of the reconstructed high speed solar wind. The SMEI analyses certify that the brightness enhancements observed behind shocks identified and measured in situ near Earth are a direct response to the plasma density enhancements that follow the shocked plasma"

---
MARKER : "2010_sw12_aip_1216_408"
TYPE   : "in_proceedings"
AUTHOR : "Kahler, S., Webb, D."
TITLE  : "Tracking nonradial motions and azimuthal expansions of interplanetary CMEs with the Solar Mass Ejection Imager"
EDITOR : "Maksimovic, M., Issautier, K., Meyer-Vernet, N., Moncuquet, M., Pantellini, F."
CTITLE : "Solar Wind Twelve"
SERIAL : "AIP Conf. Proc."
VOLUME : "1216"
PAGE   : "408-411"
YEAR   : "2010-03"
DOI    : "10.1063/1.3395889"
TOPKEY : "Coriolis-SMEI"

---
MARKER : "2010_sw12_aip_1216_355"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Bisi, M.M., Jackson, B.V., Hick, P.P., Clover, J.M., Hamilton, S., Tokumaru, M., Fujiki, K."
TITLE  : "Large-scale heliospheric structure during solar-minimum conditions using a 3D time-dependent reconstruction solar-wind model and STELab IPS observations"
EDITOR : "Maksimovic, M., Issautier, K., Meyer-Vernet, N., Moncuquet, M., Pantellini, F."
CTITLE : "Solar Wind Twelve"
SERIAL : "AIP Conf. Proc."
VOLUME : "1216"
PAGE   : "355-358"
YEAR   : "2010-03"
DOI    : "10.1063/1.3395873"
TOPKEY : "IPS"
ABS    : "Interplanetary scintillation (IPS) observations provide information about a large portion of the inner heliosphere. We have used Solar-Terrestrial Environment Laboratory (STELab) IPS velocity and g-level observations with our three-dimensional (3D) reconstruction model to determine velocities and densities of the inner heliosphere in three dimensions. We present these observations using synoptic maps generated from our time-dependent model that can measure changes with durations of less than one day. These synopses show large-scale stable solar-wind structure during solar-minimum conditions in relation to transients that are present during this period. These are also available as differences relative to the background. Here, we concentrate primarily on data covering the 2007-2009 International Heliophysical Year (IHY)."

---
MARKER : "2009_ann_geophys_27_4479"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Bisi, M.M., Jackson, B.V., Clover, J.M., Manoharan, P.K., Tokumaru, M., Hick, P.P., Buffington, A."
TITLE  : "3D reconstructions of the early-November 2004 CDAW geomagnetic storms: analysis of Ooty IPS speed and density data"
EDITOR : "Forsyth, R., Harrison, R., Luhmann, J., Fleck, B., St Cyr, C."
CTITLE : "Three eyes on the Sun - Multi-spacecraft studies of the corona and impacts on the heliosphere (STEREO-3/SOHO-22 workshop)"
SERIAL : "Ann. Geophys."
VOLUME : "27"
PAGE   : "4479-4489"
YEAR   : "2009-12"
DOI    : "10.5194/angeo-27-4479-2009"
TOPKEY : "IPS"
ABS    : "Interplanetary scintillation (IPS) remote-sensing observations provide a view of the solar wind covering a wide range of heliographic latitudes and heliocentric distances from the Sun between ~0.1 AU and 3.0 AU. Such observations are used to study the development of solar coronal transients and the solar wind while propagating out through interplanetary space. They can also be used to measure the inner-heliospheric response to the passage of coronal mass ejections (CMEs) and co-rotating heliospheric structures. IPS observations can, in general, provide a speed estimate of the heliospheric material crossing the observing line of site; some radio antennas/arrays can also provide a radio scintillation level. We use a three-dimensional (3-D) reconstruction technique which obtains perspective views from outward-flowing solar wind and co-rotating structure as observed from Earth by iteratively fitting a kinematic solar wind model to these data. Using this 3-D modelling technique, we are able to reconstruct the velocity and density of CMEs as they travel through interplanetary space. For the time-dependent model used here with IPS data taken from the Ootacamund (Ooty) Radio Telescope (ORT) in India, the digital resolution of the tomography is 10° by 10° in both latitude and longitude with a half-day time cadence. Typically however, the resolutions range from 10° to 20° in latitude and longitude, with a half- to one-day time cadence for IPS data dependant upon how much data are used as input to the tomography. We compare reconstructed structures during early-November 2004 with in-situ measurements from the Wind spacecraft orbiting the Sun-Earth L1-Point to validate the 3-D tomographic reconstruction results and comment on how these improve upon prior reconstructions."

---
MARKER : "2009_ann_geophys_27_4097"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Hick, P.P., Buffington, A., Bisi, M.M., Clover, J.M."
TITLE  : "SMEI direct, 3-D-reconstruction sky maps, and volumetric analyses, and their comparison with SOHO and STEREO observations"
EDITOR : "Forsyth, R., Harrison, R., Luhmann, J., Fleck, B., St Cyr, C."
CTITLE : "Three Eyes on the Sun - Multi-spacecraft studies of the corona and impacts on the heliosphere (STEREO-3/SOHO-22 Workshop)"
SERIAL : "Ann. Geophys."
VOLUME : "27"
PAGE   : "4097-4104"
YEAR   : "2009-11"
DOI    : "10.5194/angeo-27-4097-2009"
TOPKEY : "Coriolis-SMEI"
ABS    : "In this paper we present the results of the analysis of the late January 2007 Coronal Mass Ejection (CME) events recorded by the Solar Mass Ejection Imager (SMEI), the Solar TErrestrial RElations Observatory (STEREO), and the SOlar and Heliospheric Observatory (SOHO) spacecraft. This period occurs when the two STEREO spacecraft views are from close to Earth, and thus the views from both SMEI and the STEREO outer Heliospheric Imagers (HI-2s) coincide. Three-dimensional (3-D) analyses derived from SMEI data show many CMEs that have also been studied by others using short-term image subtractions (image-differencing techniques). During this interval we map several CME structures that are observed in both SMEI and the STEREO-A HI instruments. SMEI brightness analyses provided by short-term image subtractions ('difference images') and, alternatively, subtractions of a mean-brightness fit over a long-time duration, both show the extents of the CMEs travelling outward above the East limb that erupted from the Sun on 24 and 25 January 2007. The SMEI 3-D-reconstructions not only enhance distinct features within the CME events, but also reconcile difference-imaging results with those where a long-term base has been removed. In the January 2007 example the structure as mapped by CME difference images traces the sharp intensity gradients at the front of the CMEs; generally brighter ejected material follows behind the location of the CME front, but shows poorly in these because of its larger angular extent. Using the long-duration background removal enables SMEI's 3-D analysis to determine a mass for this CME sequence North of the ecliptic."

---
MARKER : "2009_ssr_147_89"
TYPE   : "in_journal "
AUTHOR : "Howard, T.A., Tappin, S.J."
TITLE  : "Interplanetary coronal mass ejections observed in the heliosphere: 3. Physical implications"
SERIAL : "Space Sci. Rev."
VOLUME : "147"
PAGE   : "89-110"
YEAR   : "2009-10"
DOI    : "10.1007/s11214-009-9577-7"
TOPKEY : "Coriolis-SMEI"
ABS    : "We conclude the heliospheric image series with this third and final instalment, where we consider the physical implications of our reconstruction of interplanetary coronal mass ejections from heliospheric imagers. In Paper 1 a review of the theoretical framework for the appearance of ICMEs in the heliosphere was presented and in Paper 2 a model was developed that extracted the three-dimensional structure and kinematics of interplanetary coronal mass ejections directly from SMEI images. Here we extend the model to include STEREO Heliospheric Imager data and reproduce the three-dimensional structure and kinematic evolution of a single Earth-directed interplanetary coronal mass ejection that was observed in November 2007. These measurements were made with each spacecraft independently using leading edge measurements obtained from each instrument. We found that when data from the three instruments was treated as a single collective, we were able to reproduce an estimate of the ICME structure and trajectory. There were some disparities between the modelled ICME and the in situ data, and we interpret this as a combination of a slightly more than spherically curved ICME structure and a corotating interaction region brought about by the creation of a coronal hole from the CME eruption. This is the first time evidence for such a structure has been presented and we believe that it is likely that many ICMEs are of this nature."

---
MARKER : "2009_spie_74380O"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Buffington, A., Bach, K.G., Bach, B.W, Bach, E.K., Bisi, M.M., Hick, P.P., Jackson, B.V., Klupar, P.D."
TITLE  : "Fabrication and test of a diamond-turned mirror suitable for a spaceborne photometric heliospheric imager"
EDITOR : "Fineschi, S., Fennelly, J."
CTITLE : "Solar physics and space weather instrumentation III"
SERIAL : "Proc. SPIE"
VOLUME : "7438"
PAGE   : "74380O"
YEAR   : "2009-09"
DOI    : "10.1117/12.825362"
TOPKEY : "Coriolis-SMEI, heliospheric imaging"
ABS    : "We have fabricated a diamond-turned low-mass version of a toroidal mirror which is a key element for a spaceborne visible-light heliospheric imager. This mirror's virtual image of roughly a hemisphere of sky is viewed by a conventional photometric camera. The optical system views close to the edge of an external protective baffle and does not protrude from the protected volume. The sky-brightness dynamic range and background-light rejection requires minimal wideangle scattering from the mirror surface. We describe the manufacturing process for this mirror, and present preliminary laboratory measurements of its wide-angle scattering characteristics."

---
MARKER : "2009_spie_74380N"
TYPE   : "in_proceedings"
AUTHOR : "Johnston, J.C., Webb, D.F., Norquist, D.C., Kuchar, T.A."
TITLE  : "Imaging coronal mass ejections and other heliospheric phenomena: six years of observations and implications for future capabilities"
EDITOR : "Fineschi, S., Fennelly, J."
CTITLE : "Solar Physics and Space Weather Instrumentation III"
SERIAL : "Proc. SPIE"
VOLUME : "7438"
PAGE   : "74380N"
YEAR   : "2009-09"
DOI    : "10.1117/12.828664"
TOPKEY : "Coriolis-SMEI"
ABS    : "January 2009 marked the 6th anniversary of the launch of the Air Force Research Laboratory Solar Mass Ejection Imager (SMEI) instrument on the Coriolis spacecraft. Originally planned as a three year mission, SMEI has amassed an unprecedented dataset of ~25,000 full-sky images since 2003 with a 102-minute cadence, 1° spatial resolution, and better than 8th magnitude sensitivity. SMEI, with its Sun/Earth line views, has been joined by the twin STEREO spacecraft, launched in October 2006, whose heliospheric Imagers (HIs) image along the ecliptic with opposing, off-axis views, 70° in diameter. These two data sets are complementary and several events observed by both SMEI and STEREO are being analyzed. But SMEI is nearing its end of life and the STEREO spacecraft continue to drift apart by 45°/year with decreasing telemetry coverage. What would be the characteristics of the next generation instrument in heliospheric imaging? What would the differences be for an operational instrument vs. a research instrument? What are the advantages of staring vs. composite imaging, views from the Sun/Earth line vs. other views, L1 position vs. low Earth orbit, etc? What are the engineering lessons learned from SMEI and STEREO and the environment through which such an instrument operates? In this presentation we discuss these issues and some possible future mission concepts."

---
MARKER : "2009_icarus_203_124"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Buffington, A., Bisi, M.M., Clover, J.M., Hick, P.P., Jackson, B.V., Kuchar, T.A., Price, S.D."
TITLE  : "Measurements of the Gegenschein brightness from the Solar Mass Ejection Imager (SMEI)"
SERIAL : "Icarus"
VOLUME : "203"
PAGE   : "124-133"
YEAR   : "2009-09"
TOPKEY : "zodiacal light, Gegenschein, Coriolis-SMEI"
ABS    : "The Gegenschein is viewed by the Solar Mass Ejection Imager (SMEI), which has provided near-full-sky broadband visible-light photometric maps for over 5 years. These have an angular resolution of about 0.5° and differential photometric stability of about 1% throughout this time. When individual bright stars are removed from the maps and an empirical sidereal background subtracted, the residue is dominated by the zodiacal light. The unprecedented sky coverage and duration of these measurements enables a definitive characterization of the Gegenschein. This article describes the analysis method for these data, presents a movie with time of the Gegenschein brightness distribution, determines empirical formulae describing its average shape, and discusses its variation with time. These measurements unambiguously confirm previous reports that the Gegenschein surface-brightness distribution has a decided peak in the antisolar point, which rises above a broader background."

---
MARKER : "2009_apj_702_862"
TYPE   : "in_journal "
AUTHOR : "Tappin, S.J., Howard, T.A."
TITLE  : "Direct observation of a corotating interaction region by three spacecraft"
SERIAL : "Astrophys. J."
VOLUME : "702"
PAGE   : "862-870"
YEAR   : "2009-08"
DOI    : "10.1088/0004-637X/702/2/862"
TOPKEY : "Coriolis-SMEI"
ABS    : "White-light observations of interplanetary disturbances have been dominated by interplanetary coronal mass ejections (ICMEs). This is because the other type of disturbance, the corotating interaction region (CIR), has proved difficult to detect using white-light imagers. Recently, a number of papers have appeared presenting CIR observations using the Solar Terrestrial Relations Observatory (STEREO) Heliospheric Imagers (HIs), but have mostly only focused on a single spacecraft and imager. In this paper, we present observations of a single CIR that was observed by all three current white-light heliospheric imagers (SMEI and both STEREO HIs), as well as the in situ instruments on both STEREO satellites and ACE. We begin with a discussion of the geometry of the CIR structure, and show how the apparent leading edge structure is expected to change as it corotates relative to the observer. We use these calculations to predict elongation-time profiles for CIRs of different speeds for each of the imagers, and also to predict the arrival times at the in situ instruments. We show that although all three measured different parts, they combine to produce a self-consistent picture of the CIR. Finally, we offer some thoughts on why CIRs have proved so difficult to detect in white-light heliospheric images."

---
MARKER : "2009_solar_phys_259_179"
TYPE   : "in_journal "
AUTHOR : "Morrill, J.S., Howard, R.A., Vourlidas, A., Webb, D.F., Kunkel, V."
TITLE  : "The impact of geometry on observations of CME brightness and propagation"
SERIAL : "Solar Phys."
VOLUME : "259"
PAGE   : "179-197"
YEAR   : "2009-07"
DOI    : "10.1007/s11207-009-9403-0"
TOPKEY : "Coriolis-SMEI"
ABS    : "Coronal mass ejections (CMEs) have a significant impact on space weather and geomagnetic storms and so have been the subject of numerous studies. Most CME observations have been made while these events are near the Sun (e.g., SOHO/LASCO). Recent data from the Coriolis/SMEI and STEREO/SECCHI-HI instruments have imaged CMEs farther into the heliosphere. Analyses of CME observations near the Sun measure the properties of these events by assuming that the emission is in the plane of the sky and hence the speed and mass are lower limits to the true values. However, this assumption cannot be used to analyze optical observations of CMEs far from the Sun, such as observations from SMEI and SECCHI-HI, since the CME source is likely to be far from the limb. In this paper we consider the geometry of observations made by LASCO, SMEI, and SECCHI. We also present results that estimate both CME speed and trajectory by fitting the CME elongations observed by these instruments. Using a constant CME speed does not generally produce profiles that fit observations at both large and small elongation, simultaneously. We include the results of a simple empirical model that alters the CME speed to an estimated value of the solar wind speed to simulate the effect of drag on the propagating CME. This change in speed improves the fit between the model and observations over a broad range of elongations."

---
MARKER : "2009_ssr_147_55"
TYPE   : "in_journal "
AUTHOR : "Tappin, S.J., Howard, T.A."
TITLE  : "Interplanetary coronal mass ejections observed in the heliosphere: 2. Model and data comparison"
SERIAL : "Space Sci. Rev."
VOLUME : "147"
PAGE   : "55-87"
YEAR   : "2009-06"
DOI    : "10.1007/s11214-009-9550-5"
TOPKEY : "Coriolis-SMEI"
ABS    : "With the recent advancements in interplanetary coronal mass ejection (ICME) imaging it is necessary to understand how heliospheric images may be interpreted, particularly at large elongation angles. Of crucial importance is how the current methods used for coronal mass ejection measurement in coronagraph images must be changed to account for the large elongations involved in the heliosphere. We present results comparing a new model of interplanetary disturbances with heliospheric image data, from the Solar Mass Ejection Imager. A database containing a range of ICMEs simulated with varying parameters describing its topology, orientation, location and speed was produced and compared with two ICMEs observed in February and December 2004. We identify the simulated ICME that best matches the data, and use the parameters required to identify their three-dimensional leading-edge structure, orientation and kinematics. By constant comparison with the data we are able to keep track of small changes to the ICME topology and kinematic properties, thus for the first time are able to monitor how the dynamic interaction between the ICME and the interplanetary medium affects ICME evolution. This is the second part of a series of three papers, where the theory behind the model is presented in an accompanying paper and the physical implications are discussed in the third part. The first part considers the effects of Thomson scattering across the entire span of the disturbance and includes its apparent geometry at large elongations. We find that the model converges reliably to a solution for both events, although we identify four separate structures during the December period. Comparing the 3-D trajectory and source location with known associated features identified with other spacecraft, we find a remarkable agreement between the model and data. We conclude with a brief discussion of the physical implications of the model."

---
MARKER : "2009_ssr_147_31"
TYPE   : "in_journal "
AUTHOR : "Howard, T.A., Tappin, S.J."
TITLE  : "Interplanetary coronal mass ejections observed in the heliosphere: 1. Review of theory"
SERIAL : "Space Sci. Rev."
VOLUME : "147"
PAGE   : "31-54"
DOI    : "10.1007/s11214-009-9542-5"
YEAR   : "2009-06"
TOPKEY : "Coriolis-SMEI"
ABS    : "With the recent advancements in interplanetary coronal mass ejection (ICME) imaging it is necessary to understand how heliospheric images may be interpreted, particularly at large elongation angles. Of crucial importance is how the current methods used for coronal mass ejection measurement in coronagraph images must be changed to account for the large elongations involved in the heliosphere. In this review of theory we build up a picture of ICME appearance and evolution at large elongations in terms of how it would appear to an observer near 1 AU from the Sun. We begin by revisiting the basics of Thomson scattering describing how ICMEs are detected, in this we attempt to clarify a number of common misconceptions. We then build up from a single electron to an integrated line of sight, consider the ICME as a collection of lines of sight and describe how a map of ICME appearance may be developed based on its appearance relative to each line of sight. Finally, we discuss how the topology of the ICME affects its observed geometry and kinematic properties, particularly at large elongations. This review is the first of a three-part series of papers, where a review of theory is presented here and a model is developed and used in subsequent papers."

---
MARKER : "2009_space_weather_7_s05002"
TYPE   : "in_journal "
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Webb, D.F., Howard, T.A., Fry, C.D., Kuchar, T.A., Mizuno, D.R., Johnston, J.C., Jackson, B.V."
TITLE  : "Studying geoeffective interplanetary coronal mass ejectinos between the Sun and Earth: Space weather implications of Solar Mass Ejection Imager observations"
SERIAL : "Space Weather"
VOLUME : "7"
PAGE   : "S05002"
YEAR   : "2009-05"
DOI    : "10.1029/2008SW000409"
TOPKEY : "Coriolis-SMEI"
ABS    : "Interplanetary coronal mass ejections (ICMEs) are the primary cause of severe space weather at Earth because they drive shocks and trigger geomagnetic storms that can damage spacecraft and ground-based systems. The Solar Mass Ejection Imager (SMEI) is a U.S. Air Force experiment with the ability to track ICMEs in white light from near the Sun to Earth and beyond, thus providing an extended observational range for forecasting storms. We summarize several studies of SMEI's detection and tracking capability, especially of the ICMEs associated with the intense (peak Dst ≤ -100 nT) geomagnetic storms that were the focus of the NASA Living With a Star Geostorm Coordinated Data Analysis Workshop. We describe the SMEI observations and analyses for the 18 intense storms observed from May 2003-2007 with adequate SMEI coverage and identified solar and interplanetary source regions. SMEI observed the associated ICMEs for 89% of these intense storms. For each event we extracted the time differences between these sets of times at 1 AU for shock arrival time, predicted ICME arrival time, onset of high-altitude aurora observed by SMEI, and storm onset. The mean intervals between successive pairs of these data were found to each be ~4 hours. On average, SMEI first detected the geoeffective ICME about 1 day in advance, yielding a prediction lead time of ~18 hours. Finally, the RMS values for the ICME-shock and storm-ICME time differences were determined, and provide at least a 1-hour improvement compared to similar observational and model-dependent studies."

---
MARKER : "2009_solar_phys_256_239"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Webb, D.F., Howard, T.A., Fry, C.D., Kuchar, T.A., Odstrcil, D., Jackson, B.V., Bisi, M.M., Harrison, R.A., Morrill, J.S., Howard, R.A., Johnston, J.C."
TITLE  : "Study of CME Propagation in the Inner Heliosphere: SOHO LASCO, SMEI and STEREO HI Observations of the January 2007 Events"
SERIAL : "Solar Phys."
VOLUME : "256 (1/2)"
PAGE   : "239-267"
YEAR   : "2009-04"
DOI    : "10.1007/s11207-009-9351-8"
TOPKEY : "Coriolis-SMEI"
ABS    : "We are investigating the geometric and kinematic characteristics of interplanetary coronal mass ejections (ICMEs) using data obtained by the LASCO coronagraphs, the Solar Mass Ejection Imager (SMEI), and the SECCHI imaging experiments on the STEREO spacecraft. The early evolution of CMEs can be tracked by the LASCO C2 and C3 and SECCHI COR1 and COR2 coronagraphs, and the HI and SMEI instruments can track their ICME counterparts through the inner heliosphere. The HI fields of view (4-90°) overlap with the SMEI field of view (> 20° to all sky) and, thus, both instrument sets can observe the same ICME. In this paper we present results for ICMEs observed on 24-29 January 2007, when the STEREO spacecraft were still near Earth so that both the SMEI and STEREO views of large ICMEs in the inner heliosphere coincided. These results include measurements of the structural and kinematic evolution of two ICMEs and comparisons with drive/drag kinematic, 3D tomographic reconstruction, the HAFv2 kinematic, and the ENLIL MHD models. We find it encouraging that the four model runs generally were in agreement on both the kinematic evolution and appearance of the events. Because it is essential to understand the effects of projection across large distances, that are not generally crucial for events observed closer to the Sun, we discuss our analysis procedure in some detail."

---
MARKER : "2009_solar_phys_256_201"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Bisi, M.M., Jackson, B.V., Buffington, A., Clover, J.M., Hick, P.P., Tokumaru, M."
TITLE  : "Low-resolution STELab IPS 3D reconstructions of the whole heliosphere interval and comparison with in-ecliptic solar wind measurements from STEREO and Wind instrumentation"
SERIAL : "Solar Phys."
VOLUME : "256"
PAGE   : "201-217"
YEAR   : "2009-04"
DOI    : "10.1007/s11207-009-9350-9"
TOPKEY : "IPS"
ABS    : "We present initial 3D tomographic reconstructions of the inner heliosphere during the Whole Heliosphere Interval (WHI) - Carrington Rotation 2068 (CR2068) - using Solar-Terrestrial Environment Laboratory (STELab) Interplanetary Scintillation (IPS) observations. Such observations have been used for over a decade to visualise and investigate the structure of the solar wind and to study in detail its various features. These features include co-rotating structures as well as transient structures moving out from the Sun. We present global reconstructions of the structure of the inner heliosphere during this time, and compare density and radial velocity with multi-point in situ spacecraft measurements in the ecliptic; namely STEREO and Wind data, as the interplanetary medium passes over the spacecraft locations. "

---
MARKER : "2009_solar_phys_254_387"
TYPE   : "in_journal"
AUTHOR : "Eyles, C.J., Harrison, R.A., Davis, C.J., Waltham, N.R., Shaughnessy, B.M., Mapson-Menard, H.C.A., Bewsher, D., Crothers, S.R., Davies, J.A., Simnett, G.M., Howard, R.A., Moses, J.D., Newmark, J.S., Socker, D.G., Halain, J.-P., Defise, J.-M., Mazy, E., Rochus, P."
TITLE  : "The Heliospheric Imagers onboard the STEREO mission"
SERIAL : "Solar Phys."
VOLUME : "254"
PAGE   : "387-446"
YEAR   : "2009-02"
DOI    : "10.1007/s11207-008-9299-0"
TOPKEY : "heliospheric imaging"
ABS    : "Mounted on the sides of two widely separated spacecraft, the two Heliospheric Imager (HI) instruments onboard NASA's STEREO mission view, for the first time, the space between the Sun and Earth. These instruments are wide-angle visible-light imagers that incorporate sufficient baffling to eliminate scattered light to the extent that the passage of solar coronal mass ejections (CMEs) through the heliosphere can be detected. Each HI instrument comprises two cameras, HI-1 and HI-2, which have 20° and 70° fields of view and are off-pointed from the Sun direction by 14.0° and 53.7°, respectively, with their optical axes aligned in the ecliptic plane. This arrangement provides coverage over solar elongation angles from 4.0° to 88.7° at the viewpoints of the two spacecraft, thereby allowing the observation of Earth-directed CMEs along the Sun -- Earth line to the vicinity of the Earth and beyond. Given the two separated platforms, this also presents the first opportunity to view the structure and evolution of CMEs in three dimensions. The STEREO spacecraft were launched from Cape Canaveral Air Force Base in late October 2006, and the HI instruments have been performing scientific observations since early 2007. The design, development, manufacture, and calibration of these unique instruments are reviewed in this paper. Mission operations, including the initial commissioning phase and the science operations phase, are described. Data processing and analysis procedures are briefly discussed, and ground-test results and in-orbit observations are used to demonstrate that the performance of the instruments meets the original scientific requirements."

---
MARKER : "2009_solar_phys_254_185"
TYPE   : "in_journal"
AUTHOR : "Brown, D.S., Bewsher, D., Eyles, C.J."
TITLE  : "Calibrating the pointing and optical parameters of the STEREO heliospheric imagers"
SERIAL : "Solar Phys."
VOLUME : "254 (1)"
PAGE   : "185-225"
YEAR   : "2009-01"
DOI    : "10.1007/s11207-008-9277-6"
TOPKEY : "heliospheric imaging"
ABS    : "The Heliospheric Imager (HI) instruments on the Solar TErrestrial RElations Observatory (STEREO) observe solar plasma as it streams out from the Sun and into the heliosphere. The telescopes point off-limb (from about 4° to 90° elongation) and so the Sun is not in the field of view. Hence, the Sun cannot be used to confirm the instrument pointing. Until now, the pointing of the instruments have been calculated using the nominal preflight instrument offsets from the STEREO spacecraft together with the spacecraft attitude data. This paper develops a new method for deriving the instrument pointing solutions, along with other optical parameters, by comparing the locations of stars identified in each HI image with the known star positions predicted from a star catalogue. The pointing and optical parameters are varied in an autonomous manner to minimise the discrepancy between the predicted and observed positions of the stars. This method is applied to all HI observations from the beginning of the mission to the end of April 2008. For the vast majority of images a good attitude solution has been obtained with a mean-squared deviation between the observed and predicted star positions of one image pixel or less. Updated values have been obtained for the instrument offsets relative to the spacecraft, and for the optical parameters of the HI cameras. With this method the HI images can be considered as 'self-calibrating', with the actual instrument offsets calculated as a byproduct. The updated pointing results and their by-products have been implemented in SolarSoft."

---
MARKER : "2008_jgr_113_a00a15"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Bisi, M.M., Hick, P.P., Buffington, A., Clover, J.M., Sun, W."
TITLE  : "Solar Mass Ejection Imager 3-D reconstruction of the 27-28 May 2003 coronal mass ejection sequence"
SERIAL : "J. Geophys. Res."
VOLUME : "113"
PAGE   : "A00A15"
YEAR   : "2008-12"
DOI    : "10.1029/2008JA013224"
TOPKEY : "Coriolis-SMEI, coronal mass ejections"
ABS    : "The Solar Mass Ejection Imager (SMEI) has recorded the inner-heliospheric response in white-light Thomson scattering for many hundreds of interplanetary coronal mass ejections (ICMEs). Some of these have been observed by the Solar and Heliospheric Observatory (SOHO) Large-Angle Spectroscopic Coronagraph (LASCO) instruments and also in situ by near-Earth spacecraft. This article presents a low-resolution three-dimensional (3-D) reconstruction of the 27-28 May 2003 halo CME event sequence observed by LASCO and later using SMEI observations; this sequence was also observed by all in situ monitors near Earth. The reconstruction derives its perspective views from outward flowing solar wind. Analysis results reveal the shape, extent, and mass of this ICME sequence as it reaches the vicinity of Earth. The extended shape has considerable detail that is compared with LASCO images and masses for this event. The 3-D reconstructed density, derived from the remote-sensed Thomson scattered brightness, is also compared with the Advanced Composition Explorer (ACE) and Wind spacecraft in situ plasma measurements. These agree well in peak and integrated total value for this ICME event sequence when an appropriately enhanced (~20%) electron number density is assumed to account for elements heavier than hydrogen in the ionized plasma."

---
MARKER : "2008_jgr_113_a00a11"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Bisi, M.M., Jackson, B.V., Hick, P.P., Buffington, A., Odstrcil, D., Clover, J.M."
TITLE  : "Three-dimensional reconstructions of the early-November 2004 Coordinated Data Analysis Workshop geomagnetic storms: Analyses of STELab IPS speed and SMEI density data"
SERIAL : "J. Geophys. Res."
VOLUME : "113"
PAGE   : "A00A11"
YEAR   : "2008-10"
DOI    : "10.1029/2008JA013222"
TOPKEY : "Coriolis-SMEI, IPS"
ABS    : "Combined interplanetary scintillation (IPS) and Solar Mass Ejection Imager (SMEI) remote-sensing observations provide a view of the solar wind at almost all heliographic latitudes and covering distances from the Sun between 0.1 AU and 3.0 AU. They are used to study the development of the solar wind and coronal transients as they move out into interplanetary space, and also the inner heliospheric response to the passage of corotating solar structures and coronal mass ejections (CMEs). The observations take place in both radio scintillation level and speed for IPS, and in Thomson-scattered white light brightness for SMEI. With colleagues at the Solar Terrestrial Environment Laboratory (STELab), Nagoya University, Japan, we have developed a data analysis system for the STELab IPS data which can also be applied to SMEI white light data. This employs a three-dimensional (3-D) reconstruction technique that obtains perspective views from solar corotating plasma and outward flowing solar wind as observed from the Earth by iterative fitting of a kinematic solar wind model to the data. This 3-D modeling technique permits reconstructions of the density and speed of CMEs and other interplanetary transients at relatively coarse spatial and temporal resolutions. For the time-dependent model (used here), these typically range from 5° to 20° in latitude and longitude, with a 1/2 to 1 day time cadence. For events during early November 2004 we compare these reconstructed structures with in situ measurements from the ACE and Wind (near-Earth) spacecraft to validate the 3-D tomographic reconstruction results and provide input to the ENLIL 3-D magnetohydrodynamic (MHD) numerical model."

---
MARKER : "2008_aa_492_167"
TYPE   : "in_journal "
AUTHOR : "Tarrant, N.J., Chaplin, W.J., Elsworth, Y.P., Spreckley, S.A., Stevens, I.R."
TITLE  : "SMEI observations of previously unseen pulsation frequencies in γ Doradus"
SERIAL : "Astron. Astrophys."
VOLUME : "492"
PAGE   : "167-169"
YEAR   : "2008-10"
DOI    : "10.1051/0004-6361:200810952"
TOPKEY : "Coriolis-SMEI"
ABS    : "Aims: As g-mode pulsators, gamma-Doradus-class stars may naively be expected to show a large number of modes. Taking advantage of the long photometric time-series generated by the Solar Mass Ejection Imager (SMEI) instrument, we have studied the star gamma Doradus to determine whether any other modes than the three already known are present at observable amplitude. Methods: High-precision photometric data from SMEI taken between April 2003 and March 2006 were subjected to periodogram analysis with the PERIOD04 package. Results: We confidently determine three additional frequencies at 1.39, 1.87, and 2.743 cycles per day. These are above and beyond the known frequencies of 1.320, 1.364, and 1.47 cycles per day. Conclusions: Two of the new frequencies, at 1.39 and 1.87 cycles per day, are speculated to be additional modes of oscillation, with the third frequency at 2.743 cycles per day a possible combination frequency."

---
MARKER : "2008_mnras_388_1239"
TYPE   : "in_journal "
AUTHOR : "Spreckley, S.A., Stevens, I.R."
TITLE  : "The period and amplitude changes of Polaris (UMi) from 2003 to 2007 measured with SMEI"
SERIAL : "Mon. Not. R. Astron. Soc."
VOLUME : "388 (3)"
PAGE   : "1239-1244"
YEAR   : "2008-08"
DOI    : "10.1111/j.1365-2966.2008.13439.x"
TOPKEY : "Coriolis-SMEI"
ABS    : "We present an analysis of 4.5 years of high precision (0.1%) space-based photometric measurements of the Cepheid variable Polaris, obtained by the broad band Solar Mass Ejection Imager (SMEI) instrument on board the Coriolis satellite. The data span from April 2003 to October 2007, with a cadence of 101 minutes and a fill factor of 70%. We have measured the mean peak to peak amplitude across the whole set of observations to be 25 mmag. There is, however, a clear trend that the size of the oscillations has been increasing during the observations, with peak to peak variations less than 22 mmag in early 2003, increasing to around 28 mmag by October 2007, suggesting that the peak to peak amplitude is increasing at a rate of 1.39 &plusmn; 0.12 mmag yr<sup>&minus;1</sup>. Additionally, we have combined our new measurements with archival measurements to measure a rate of period change of 4.90 &plusmn; 0.26 s yr <sup>&minus;1</sup> over the last 50 years. However, there is some suggestion that the period of Polaris has undergone a recent decline, and combined with the increased amplitude, this could imply evolution away from an overtone pulsation mode into the fundamental or a double pulsation mode depending on the precise mass of Polaris."

---
MARKER : "2008_jgr_113_a08102"
TYPE   : "in_journal "
AUTHOR : "Howard, T.A., Simnett, G.M."
TITLE  : "Interplanetary coronal mass ejections that are undetected by solar coronagraphs"
SERIAL : "J. Geophys. Res."
VOLUME : "113"
PAGE   : "A08102"
YEAR   : "2008-08"
DOI    : "10.1029/2007JA012920"
TOPKEY : "Coriolis-SMEI"
ABS    : "From February 2003 to September 2005 the Solar Mass Ejection Imager on the Coriolis spacecraft detected 207 interplanetary coronal mass ejections (ICME) in the inner heliosphere. We have examined the data from the Large Angle Spectroscopic Coronagraph (LASCO) on the SOHO spacecraft for evidence of coronal transient activity that might have been the solar progenitor of the Solar Mass Ejection Imager (SMEI) events, taking into account the projected speed of the SMEI event and its position angle in the plane of the sky. We found a significant number of SMEI events where there is either only a weak or unlikely coronal mass ejection (CME) detected by LASCO or no event at all. A discussion of the effects of projection across large distances on the ICME measurements is made, along with a new technique called the Cube-Fit procedure that was designed to model the ICME trajectory more accurately than simple linear fits to elongation-time plots. Of the 207 SMEI events, 189 occurred during periods of full LASCO data coverage. Of these, 32 or 17% were found to have a weak or unlikely LASCO counterpart, and 14 or 7% had no apparent LASCO transient association. Using solar X-ray, EUV and H&alpha; data we investigated three main physical possibilities for ICME occurrence with no LASCO counterpart: (1) Corotating interaction regions (CIRs), (2) erupting magnetic structures (EMS), and (3) flare blast waves. We find that only one event may possibly be a CIR and that flare blast waves can be ruled out. The most likely phenomenon is investigated and discussed, that of EMS. Here, the transient erupts in the same manner as a typical CME, except that they do not have sufficient mass to be detected by LASCO. As the structure moves outward, it accumulates and concentrates solar wind material until it is bright enough to be detected by SMEI."

---
MARKER : "2008_apj_683_433"
TYPE   : "in_journal"
AUTHOR : "Bruntt, H., Evans, N.R., Stello, D., Penny, A.J., Eaton, J.A., Buzasi, D.L., Sasselov, D.D., Preston, H.L., Miller-Ricci, E."
TITLE  : "Polaris the Cepheid returns: 4.5 years of monitoring from ground and space"
SERIAL : "Astrophys. J."
VOLUME : "683"
PAGE   : "433-440"
YEAR   : "2008-08"
DOI    : "10.1086/589565"
TOPKEY : "Coriolis-SMEI"
ABS    : "We present the analysis of 4.5 years of nearly continuous observations of the classical Cepheid Polaris, which comprise the most precise data available for this star. We have made spectroscopic measurements from ground and photometric measurements from the WIRE star tracker and the SMEI instrument on the Coriolis satellite. Measurements of the amplitude of the dominant oscillation (P = 4 days), that go back more than a century, show a decrease from 120 mmag to 30 mmag (V magnitude) around the turn of the millennium. It has been speculated that the reason for the decrease in amplitude is the evolution of Polaris towards the edge of the instability strip. However, our new data reveal an increase in the amplitude by about 30% from 2003-2006. It now appears that the amplitude change is cyclic rather than monotonic, and most likely the result of a pulsation phenomenon. In addition, previous radial velocity campaigns have claimed the detection of long-period variation in Polaris (P &gt; 40 days). Our radial velocity data are more precise than previous datasets, and we find no evidence for additional variation for periods in the range 3-50 days with an upper limit of 100 m/s. However, in the WIRE data we find evidence of variation on time-scales of 2-6 days, which we interpret as being due to granulation."

---
MARKER : "2008_apj_683_l79"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Breen, A.R., Fallows, R.A., Bisi, M.M., Jones, R.A., Jackson, B.V., Kojima, M., Dorrian, G.D., Middleton, H.R., Thomasson, P., Wannberg, G."
TITLE  : "The solar eruption of 2005 May 13 and its effects: Long-baseline interplanetary scintillation observations of the Earth-directed coronal mass ejection"
SERIAL : "Astrophys. J. Lett."
VOLUME : "683"
PAGE   : "L79-L82"
YEAR   : "2008-08"
DOI    : "10.1086/591520"
TOPKEY : "IPS"
ABS    : "Long-baseline observations of interplanetary scintillation (IPS) provide a unique source of information on solar wind speed and meridional direction across the inner regions of the solar system. We report the results of a series of coordinated IPS observations of an Earth-directed CME. A significant development in the interpretation of these data is the use of 3D tomographic reconstructions of solar wind structure derived from STELab IPS data to better constrain the analysis of extremely long baseline observations from EISCAT and MERLIN. The combination of these two approaches leads to a significantly better understanding of the interaction of the CME with the background solar wind than would be possible with either technique alone, revealing a significant rotation in the meridional flow direction of the background wind associated with the passage of the CME. The CME itself is decelerated significantly between its emergence through the corona and its arrival in the IPS ray path, with comparatively little change in speed from then until arrival at ACE."

---
MARKER : "2008_aa_483_l43"
TYPE   : "in_journal "
AUTHOR : "Tarrant, N.J., Chaplin, W.J., Elsworth, Y., Spreckley, S.A., Stevens, I.R."
TITLE  : "Oscillations in beta Ursae Minoris: Observations with SMEI"
SERIAL : "Astron. Astrophys."
VOLUME : "483"
PAGE   : "L43"
YEAR   : "2008-06"
DOI    : "10.1051/0004-6361:200809738"
TOPKEY : "Coriolis-SMEI"
ABS    : "<i>Aims</i>. From observations of the K4III star &beta; UMi we attempt to determine whether oscillations or any other form of variability is present.<br /> <i>Methods</i>. A high-quality photometric time series of ~1000 days in length obtained from the SMEI instrument on the Coriolis satellite is analysed. Various statistical tests were performed to determine the significance of features seen in the power density spectrum of the light curve.<br /> <i>Results</i>. Two oscillations with frequencies 2.44 and 2.92 &mu;Hz have been identified. We interpret these oscillations as consecutive overtones of an acoustic spectrum, implying a large frequency spacing of 0.48 &mu;Hz. Using derived asteroseismic parameters in combination with known astrophysical parameters, we estimate the mass of &beta; UMi to be 1.3&plusmn;0.3 M<sub>Sun</sub>. Peaks of the oscillations in the power density spectrum show width, implying that modes are stochastically excited and damped by convection. The mode lifetime is estimated at 18&plusmn;9 days."

---
MARKER : "2008_aa_482_l1"
TYPE   : "in_journal"
AUTHOR : "Read, A.M., Saxton, R.D., Torres, M.A.P., Esquej, P., Kuulkers, E., Jonker, P.G., Osborne, J.P., Freyberg, M.J., Challis, P."
TITLE  : "XMM-Newton slew survey discovery of the nova XMMSL1 J070542.7-381442 (V598 Puppis)"
SERIAL : "Astron. Astrophys."
VOLUME : "482"
PAGE   : "L1-L4"
YEAR   : "2008-05"
DOI    : "10.1051/0004-6361:200809456"
TOPKEY : "novae"
ABS    : "Aims. In an attempt to catch new X-ray transients while they are still bright, the data taken by XMM-Newton as it slews between targets are being processed and cross-correlated with other X-ray observations as soon as the slew data appear in the XMM-Newton archive.
Methods. A bright source, XMMSL1 J070542.7-381442, was detected on 9 Oct. 2007 at a position where no previous X-ray source had been seen. The XMM slew data and optical data acquired with the Magellan Clay 6.5 m telescope were used to classify the new object.

Results. No XMM slew X-ray counts are detected above 1 keV and the source is seen to be ~750 times brighter than the ROSAT All-Sky Survey upper limit at that position. The normally m_V ~ 16 star, USNO-A2.0 0450-03360039, which lies 3.5'' from the X-ray position, was seen in our Magellan data to be very much enhanced in brightness. Our optical spectrum showed emission lines that identified the source as a nova in the auroral phase; hence, this optical source is undoubtedly the progenitor of the X-ray source - a new nova (now also known as V598 Pup). The X-ray spectrum indicates that the nova was in a super-soft state (with kT_eff ~ 35 eV). We estimate the distance to the nova to be ~3 kpc. Analysis of archival robotic optical survey data shows a rapid-decline light curve consistent with what is expected for a very fast nova.

Conclusions. The XMM-Newton slew data present a powerful opportunity to find new X-ray transient objects while they are still bright. Here we present the first such source discovered by the analysis of near real-time slew data."

---
MARKER : "2008_aspcs_385_167"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Odstrcil, D., Pizzo, V.J., Arge, C.N., Bisi, M.M., Hick, P.P., Jackson, B.V., Ledvina, S.A., Luhmann, J.G., Linker, J.A., Mikic, Z., Riley, P."
TITLE  : "Numerical simulations of solar wind disturbances by coupled models"
EDITOR : "Pogorelov, N.V., Edouard, A., Zank, G.P."
CTITLE : "Numerical modeling of space plasma flows: Astronum-2007"
SERIAL : "ASP Conf. Series"
VOLUME : "385"
PAGE   : "167"
YEAR   : "2008"
URL    : "http://www.aspbooks.org/a/volumes/article_details/?paper_id=28176"
TOPKEY : "coronal mass ejections, interplanetary shocks"
ABS    : "Numerical modeling plays a critical role in efforts to understand the connection between solar eruptive phenomena and their impacts in the near-Earth space environment and in interplanetary space. Coupling the heliospheric model with empirical, observational, and numerical coronal models is described. Results show background solar wind, evolution of interplanetary transients, connectivity of magnetic field lines, and interplanetary shocks approaching geospace."

---
MARKER : "2008_apj_677_798"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Buffington, A., Bisi, M.M., Clover, J.M., Hick, P.P., Jackson, B.V., Kuchar, T.A."
TITLE  : "Analysis of plasma-tail motions for comets C/2001 Q4 (NEAT) and C/2002 T7 (LINEAR) using observations from SMEI"
SERIAL : "Astrophys. J."
VOLUME : "677"
PAGE   : "798-807"
YEAR   : "2008-04"
DOI    : "10.1086/529039"
TOPKEY : "Coriolis-SMEI, comet plasma tail, solar wind"
ABS    : "Comets C/2001 Q4 (NEAT) and C/2002 T7 (LINEAR) passed within ~0.3 AU of Earth in April and May of 2004. Their tails were observed by the Earth-orbiting Solar Mass Ejection Imager (SMEI) during this period. A time series of photometric SMEI sky maps displays the motions and frequent disruptions of the comet plasma tails. Ephemerides are used to unfold the observing geometry; the tails are often seen to extend ~0.5 AU from the comet nuclei. Having selected 12 of the more prominent motions as 'events' for further study, we introduce a new method for determining solar wind radial velocities from these SMEI observations. We find little correlation between these and the changing solar wind parameters as measured close to Earth, or with coarse three-dimensional reconstructions using interplanetary scintillation data. A likely explanation is that the transverse sizes of the solar wind perturbations responsible for these disruptions are small, less < 0.05 AU. We determine the radial velocities of these events during the disruptions, using a technique only possible when the observed comet tails extend over a significant fraction of an AU. We find typical radial velocities during these events of 50-100 km s^-1 lower than before or afterward. Time durations of such events vary, typically from 3 to 8 hr, and correspond to comet traversal distances ~106 km (0.007 AU). We conclude that these large disturbances are primarily due to ubiquitous solar wind flow variations, of which these measured events are a subset."

---
MARKER : "2008_jgr_113_a04101"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Kuchar, T.A., Buffington, A., Arge, C.N., Hick, P.P., Howard, T.A., Jackson, B.V., Johnston, J.C., Mizuno, D.R., Tappin, S.J., Webb, D.F."
TITLE  : "Observations of a comet tail disruption induced by the passage of a CME"
SERIAL : "J. Geophys. Res."
VOLUME : "113"
PAGE   : "A04101"
YEAR   : "2008-04"
DOI    : "10.1029/2007JA012603"
TOPKEY : "Coriolis-SMEI, comet plasma tail, coronal mass ejections"
ABS    : "The Solar Mass Ejection Imager observed an extremely faint interplanetary coronal mass ejection (ICME) as it passed Comet C/2001 Q4 (NEAT) on 5 May 2004, apparently causing a disruption of its plasma tail. This is the first time that an ICME has been directly observed interacting with a comet. SMEI's nearly all-sky coverage and image cadence afforded unprecedented coverage of this rarely observed event. The onset first appeared as a 'kink' moving antisunward that eventually developed knots within the disturbed tail. These knots appeared to be swept up in the solar wind flow. We present the SMEI observations as well as identify a likely SOHO/LASCO progenitor of the CME. SMEI observed two other comets (C/2002 T7 [LINEAR] and C/2004 F4 [Bradfield]) and at least five similar events during a 35-d period encompassing this observation. Although these had similar morphologies to the 5 May NEAT event, SMEI did not observe any ICMEs in these cases. Three of these were observed close to the heliospheric current sheet indicating that a magnetic boundary crossing may have contributed to the disruptions. However, there are no discernable causes in the SMEI observations for the remaining two events."

---
MARKER : "2008_solar_phys_248_213"
TYPE   : "in_journal"
AUTHOR : "Auchere, F., Soubrie, E., Bocchialini, K., LeGall, F."
TITLE  : "FESTIVAL: A multiscale visualization tool for solar imaging data"
SERIAL : "Solar Phys."
VOLUME : "248"
PAGE   : "213-224"
YEAR   : "2008-04"
DOI    : "10.1007/s11207-008-9163-2"
TOPKEY : "heliospheric imaging"
ABS    : "Since 4 December 2006, the SECCHI instrument suites onboard the two STEREO A and B probes have been imaging the solar corona and the heliosphere on a wide range of angular scales. The EUVI telescopes have a plate scale of 1.7 arcseconds/pixel, while that of the HI2 wide-angle cameras is 2.15 arcminutes/pixel, i.e. 75 times larger, with the COR1 and COR2 coronagraphs having intermediate plate scales. These very different instruments, aimed at studying Coronal Mass Ejections and their propagation in the heliosphere, create a data visualization challenge. This paper presents FESTIVAL, a SolarSoftware package originally developed to be able to map the SECCHI data into dynamic composite images of the sky as seen by the STEREO and SOHO probes. Data from other imaging instruments can also be displayed. Using the mouse, the user can quickly and easily zoom in and out and pan through these composite images to explore all spatial scales from EUVI to HI2 while keeping the native resolution of the original data. A large variety of numerical filters can be applied, and additional data (i.e. coordinate grids, stars catalogs, etc.) can be overlaid on the images. The architecture of FESTIVAL is such that it is easy to add support for other instruments and these new data immediately benefit from the already existing capabilities. Also, because its mapping engine is fully 3D, FESTIVAL provides a convenient environment to display images from future out-of-the-Ecliptic solar missions, such as Solar Orbiter or Solar Probe."

---
MARKER : "2008_space_weather_6_s03006"
TYPE   : "in_journal "
AUTHOR : "Sun, W., Deehr, C.S., Dryer, M., Fry, C.D., Smith, Z.K., Akasofu, S.-I."
TITLE  : "Simulated Solar Mass Ejection Imager and 'Solar Terrestrial Relations Observatory-like' views of the solar wind following the solar flares of 27-29 May 2003"
SERIAL : "Space Weather"
VOLUME : "6"
PAGE   : "S03006"
YEAR   : "2008-03"
DOI    : "10.1029/2006SW000298"
TOPKEY : "Coriolis-SMEI"
ABS    : "The three-dimensional Hakamada-Akasofu-Fry (HAFv.2) kinematic solar wind model can be extended to predict what the Solar Terrestrial Relations Observatory (STEREO) spacecraft might expect in observing large-scale plasma clouds ejected from the Sun. In order to demonstrate this capability, the HAFv.2 model was used to simulate the first observations of a halo coronal mass ejection (CME) from the Solar Mass Ejection Imager (SMEI) instrument on the Coriolis spacecraft, acquired after the solar events of 27-29 May 2003. Projections of the Thomson-scattered white light intensity on the plane of sky, as observed by the SMEI cameras, were calculated from the three-dimensional simulations. These simulations of the background solar wind and two shock fronts compare favorably with the white light observations of plasma clouds by the SMEI instrument. The method thus developed is then applied to hypothetical locations of the STEREO spacecraft in a later phase of the STEREO mission. It is shown that the model can be a valuable aid and guide in the identification of multiple shock-induced variations of the solar wind."

---
MARKER : "2008_solar_phys_247_171"
TYPE   : "in_journal "
AUTHOR : "Harrison, R.A., Davis, C.J., Eyles, C.J., Bewsher, D., Crothers, S., Davies, J.A., Howard, R.A., Moses, D.J., Socker, D.G., Halain, J.-P., Defise, J.-M., Mazy, E., Rochus, P., Webb, D.F., Simnett, G.M."
TITLE  : "First imaging of coronal mass ejections in the heliosphere viewed from outside the Sun-Earth line"
SERIAL : "Solar Phys."
VOLUME : "247"
PAGE   : "171-193"
YEAR   : "2008-01"
DOI    : "10.1007/s11207-007-9083-6"
TOPKEY : "Coriolis-SMEI"
ABS    : "We show for the first time images of solar coronal mass ejections (CMEs) viewed using the Heliospheric Imager (HI) instrument aboard the NASA STEREO spacecraft. The HI instruments are wide-angle imaging systems designed to detect CMEs in the heliosphere, in particular, for the first time, observing the propagation of such events along the Sun-Earth line, that is, those directed towards Earth. At the time of writing the STEREO spacecraft are still close to the Earth and the full advantage of the HI dual-imaging has yet to be realised. However, even these early results show that despite severe technical challenges in their design and implementation, the HI instruments can successfully detect CMEs in the heliosphere, and this is an extremely important milestone for CME research. For the principal event being analysed here we demonstrate an ability to track a CME from the corona to over 40 degrees. The time-altitude history shows a constant speed of ascent over at least the first 50 solar radii and some evidence for deceleration at distances of over 20 degrees. Comparisons of associated coronagraph data and the HI images show that the basic structure of the CME remains clearly intact as it propagates from the corona into the heliosphere. Extracting the CME signal requires a consideration of the F-coronal intensity distribution, which can be identified from the HI data. Thus we present the preliminary results on this measured F-coronal intensity and compare these to the modelled F-corona of Koutchmy and Lamy (IAU Colloq. 85, 63, 1985). This analysis demonstrates that CME material some two orders of magnitude weaker than the F-corona can be detected; a specific example at 40 solar radii revealed CME intensities as low as 1.7&times;10^-14 of the solar brightness. These observations herald a new era in CME research as we extend our capability for tracking, in particular, Earth-directed CMEs into the heliosphere."

---
MARKER : "2007_solar_phys_246_393"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "The misnomer of 'post-flare loops'"
SERIAL : "Solar Phys."
VOLUME : "246 (2)"
PAGE   : "393-397"
YEAR   : "2007-12"
DOI    : "10.1007/s11207-007-9088-1"
REMARK : "Five earlier essays published in EOS?"
TOPKEY : "flares"
ABS    : "Attention is drawn to the fact that the term 'post-flare loops' is incorrect and should be avoided, because the loops are parts of the flare itself. Two other names for these loop systems are suggested."

---
MARKER : "2007_jgr_112_a10102_correction"
TYPE   : "in_journal"
AUTHOR : "Zhang, J., Richardson, I.G., Webb, D.F., Gopalswamy, N., Huttunen, E., Kasper, J., Nitta, N.V., Poomvises, W., Thompson, B.J., Wu, C.-C., Yashiro, S., Zhukov, A.N."
TITLE  : "Correction to 'Solar and interplanetary sources of major geomagnetic storms (Dst &le; -100 nT) during 1996-2005'"
SERIAL : "J. Geophys. Res."
VOLUME : "112 (A12)"
PAGE   : "A12103"
YEAR   : "2007-12"
DOI    : "10.1029/2007JA012891"
TOPKEY : "Coriolis-SMEI"
ABS    : "In the paper 'Solar and interplanetary sources of major geomagnetic storms (Dst &lt; 100 nT) during 1996-2005' by J. Zhang et al. (Journal of Geophysical Research, 112, A09209, doi:10.1029/2007JA012321, 2007) Table 1 had some errors. The correct table is reproduced here."

---
MARKER : "2007_aat_26_477"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Hick, P.P., Buffington, A., Bisi, M.M., Kojima, M., Tokumaru, M."
TITLE  : "Comparison of the extent and mass of CME events in the interplanetary medium using IPS and SMEI Thomson scattering observations"
EDITOR : "Chasei, I., Shishov, V."
CTITLE : "Scattering and scintillation in radio astronomy"
SERIAL : "Astron. Astrophys. Trans."
VOLUME : "26 (6)"
PAGE   : "477-487"
YEAR   : "2007-12"
DOI    : "10.1080/10556790701612221"
TOPKEY : "IPS, Coriolis-SMEI, coronal mass ejections"
ABS    : "The Solar-Terrestrial Environment Laboratory (STELab), Japan, interplanetary scintillation (IPS) g-level and velocity measurements can be used to give the extent of CME disturbances in the interplanetary medium arising from the scattering of the radio waves from distant point-like natural sources through the intervening medium. In addition, white-light Thomson-scattering observations from the Solar Mass Ejection Imager (SMEI) have recorded the inner heliospheric response to several hundred CMEs. The work described here compares and details the difference in three-dimensional (3D) reconstructions for these two data sets for the well-observed 28 October 2003 halo CME seen in LASCO; this passed Earth on 29 October in the SMEI data at the same elongations as IPS g-level observations. The SMEI data analysis employs a 3D tomographic reconstruction technique that obtains perspective views from outward-flowing solar wind as observed from Earth, iteratively fitting a kinematic solar wind density model, and when available, including IPS velocity data. This technique improves the separation of the heliospheric response in SMEI from other sources of background noise, and also provides the 3D structure of the CME and its mass. The analysis shows and tracks outward the northward portion of a loop structure of this halo CME. We determine an excess mass for this structure of 6.7 10^16 g and a total mass of 8.3 10^16 g in the SMEI analysis, and these are comparable to values obtained using IPS g-level data and a 3D reconstruction technique developed for these data and applied to this event. We also extend further the application for these analyses."

---
MARKER : "2007_aat_26_467"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Kojima, M., Tokumaru, M., Fujiki, K., Hayashi, L., Jackson, B.V."
TITLE  : "IPS tomographic observations of 3D solar wind structure"
EDITOR : "Chasei, I., Shishov, V."
CTITLE : "Scattering and Scintillation in Radio Astronomy"
SERIAL : "Astronomical and Astrophysical Transactions"
VOLUME : "26 (6)"
PAGE   : "467-476"
YEAR   : "2007-12"
DOI    : "10.1080/10556790701596200"
TOPKEY : "IPS"
ABS    : "Interplanetary scintillation (IPS) observations have been improved by development of deconvolution methods for the line-of-sight integration effect. One deconvolution method is to use a computer-assisted tomographic analysis (CAT) technique. In this work, four different kinds of CAT method have been developed. Two of them can be applied to stable solar wind structure in the solar minimum phase, one to quasi-stable solar wind, and the other can derive the three-dimensional structure of transient solar wind events, such as a CME. IPS measurements have enough spatial resolution and accuracy to collaborate with spacecraft observations and theoretical studies of the solar wind. Here, these computer assisted tomographic deconvolution methods are introduced and their application to solar wind studies is described."

---
MARKER : "2007_aat_26_489"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Fallows, R.A., Breen, A.R., Bisi, M.M., Jones, R.A., Dorrian, G.D."
TITLE  : "Interplanetary Scintillation Using EISCAT and MERLIN: Extremely-Long Baselines at Multiple Frequencies"
EDITOR : "Chasei, I., Shishov, V."
CTITLE : "Scattering and Scintillation in Radio Astronomy"
SERIAL : "Astronomical and Astrophysical Transactions"
VOLUME : "26 (6)"
PAGE   : "489-500"
YEAR   : "2007-12"
DOI    : "10.1080/10556790701612197"
TOPKEY : "IPS"
ABS    : "Improvements to two of the radio telescopes of European Incoherent SCATter radar (EISCAT) allow measurements of Interplanetary Scintillation (IPS) at 1.4 GHz, and this has prompted two major developments in studies of IPS. Simultaneous observations between EISCAT and MERLIN allow baselines of up to 2000 km, significantly improving velocity resolution and making possible much greater accuracy in determining the direction of flow than previously, as well as demonstrating that density variations in the slow solar wind remain partially correlated for at least 8 s. Initial results suggest two fast solar wind modes, and there is evidence for super-radial (meridional) expansion of the fast solar wind. Trials have been conducted using different observing frequencies at different sites, including the use of the EISCAT Svalbard Radar for IPS for the first time. Observations at 500, 928 and 1420 MHz with baselines of up to 1200 km have been carried out. The results are found to be consistent between single- and dual-frequency correlations, allowing the range of observations possible with the EISCAT system to be expanded."

---
MARKER : "2007_adv_geosci_st_14_161"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Bisi, M.M., Jackson, B.V., Hick, P.P., Buffington, A., Clover, J.M."
TITLE  : "Coronal mass ejection reconstructions from interplanetary scintillation data using a kinematic model: a brief review"
EDITOR : "Duldig, M."
CTITLE : "Proc. AOGS 2007"
SERIAL : "Advances in Geosciences: Solar Terrestrial (ST)"
VOLUME : "14"
PAGE   : "161-181"
YEAR   : "2007"
DOI    : "10.1142/9789812836205_0012"
PUBLISH: "World Scientific Publ. Co"
TOPKEY : "IPS"
ABS    : "Interplanetary scintillation (IPS) observations of multiple sources provide a view of the solar wind at all heliographic latitudes from around 1 AU down to coronagraph fields of view. These are used to study the evolution of the solar wind and solar transients out into interplanetary space, and also the inner-heliospheric response to co-rotating solar structures and coronal mass ejections (CMEs). With colleagues at the Solar Terrestrial Environment Laboratory (STELab), Nagoya University, Japan, we have developed near-real-time access of STELab IPS data for use in space-weather forecasting. We use a three-dimensional (3D) reconstruction technique that obtains perspective views of solar co-rotating plasma and of outward-flowing solar wind crossing our lines of sight from the Earth to the radio sources. This is accomplished by iteratively fitting a kinematic solar wind model to the IPS observations. This 3D modeling technique permits reconstructions of the density and speed structures of CMEs and other interplanetary transients at a relatively coarse resolution. These reconstructions have a 28-day solar-rotation cadence with 10&deg; latitudinal and longitudinal heliographic resolution for a co-rotational model, and a one-day cadence and 20&deg; latitudinal and longitudinal heliographic resolution for a time-dependent model. These resolutions are restricted by the numbers of lines of sight available for the reconstructions. When Solar Mass Ejection Imager (SMEI) Thomson-scattered brightness measurements are used, lines of sight are much greater in number so that density reconstructions can be better resolved. Higher resolutions are also possible when these analyses are applied to Ootacamund IPS data."

---
MARKER : "2007_smei_final_afrl_report"
TYPE   : "tech. report"
AUTHOR : "Johnston, J.C, Holladay, P.E., Kuchar, T.A."
TITLE  : "Solar Mass Ejection Imager (SMEI) mission: Final report"
PUBLISH: "Air Force Research Laboratory"
VOLUME : "AFRL-RV-HA-TR-2007-1126"
YEAR   : "2007-10"
TOPKEY : "Coriolis-SMEI"
ABS    : "The Solar Mass Ejection Imager experiment, launched 6 January 2003 on Coriolis, continues to detect and track coronal mass ejections (CMEs). SMEI has outlived its planned 2-3 year lifetime and amassed a database of full-sky images with a 102-minute cadence recorded for almost five years. The Navy presently operates the spacecraft, provides SMEI data to AFRL, and plans to operate Coriolis for as long as its experiment, Windsat, is functional. An irrecoverable failure on its A-side electronics (March 2006) forced us to switch SMEI to B-side, which is operating nominally. Camera 3 (closest to the Sun) continually degrades with accum ulated radiation dose and has run above predicted/planned-for temperatures. Periodic anneals have helped to alleviate this problem, and a severe on-board masking of hot pixels in Camera 3 was instituted in 2006. Despite these problems, SMEI has amassed a wealth of detailed images of coronal mass ejections, high altitude auroras, variable stars, zodiacal dust, and comet tail interactions with the heliosphere. SMEI has demonstrated that such an instrument can improve space weather forecasts by 30%."

---
MARKER : "2007_jgr_112_a10102"
TYPE   : "in_journal "
AUTHOR : "Zhang, J., Richardson, I.G., Webb, D.F., Gopalswamy, N., Huttunen, E., Kasper, J.C., Nitta, N.V., Poomvises, W., Thompson, B.J., Wu, C.-C., Yashiro, S., Zhukov, A."
TITLE  : "Solar and interplanetary sources of major geomagnetic storms (Dst <= -100 nT) in 1996-2004"
SERIAL : "J. Geophys. Res."
VOLUME : "112"
PAGE   : "A10102, 1-19"
YEAR   : "2007-10"
DOI    : "10.1029/2007JA012321"
TOPKEY : "Coriolis-SMEI"
ABS    : "We present the results of an investigation of the sequence of events from the Sun to the Earth that ultimately led to the 88 major geomagnetic storms (defined by minimum Dst &le; -100 nT) that occurred during 1996-2005. The results are achieved through cooperative efforts that originated at the Living with a Star (LWS) Coordinated Data-Analysis Workshop (CDAW) held at George Mason University in March 2005. On the basis of careful examination of the complete array of solar and in situ solar wind observations, we have identified and characterized, for each major geomagnetic storm, the overall solar-interplanetary (solar-IP) source type, the time, velocity, and angular width of the source coronal mass ejection (CME), the type and heliographic location of the solar source region, the structure of the transient solar wind flow with the storm-driving component specified, the arrival time of shock/disturbance, and the start and ending times of the corresponding IP CME (ICME). The storm-driving component, which possesses a prolonged and enhanced southward magnetic field (Bs), may be an ICME, the sheath of shocked plasma (SH) upstream of an ICME, a corotating interaction region (CIR), or a combination of these structures. We classify the Solar-IP sources into three broad types: (1) S-type, in which the storm is associated with a single ICME and a single CME at the Sun; (2) M-type, in which the storm is associated with a complex solar wind flow produced by multiple interacting ICMEs arising from multiple halo CMEs launched from the Sun in a short period; (3) C-type, in which the storm is associated with a CIR formed at the leading edge of a high-speed stream originating from a solar coronal hole (CH). For the 88 major storms, the S-type, M-type, and C-type events number 53 (60%), 24 (27%), and 11 (13%), respectively. For the 85 events for which the surface source regions could be investigated, 54 (63%) of the storms originated in solar active regions, 11 (13%) in quiet Sun regions associated with quiescent filaments or filament channels, and 11 (13%) were associated with coronal holes. Remarkably, nine (11%) CME-driven events showed no sign of eruptive features on the surface or in the low corona (e.g., no flare, no coronal dimming, and no loop arcade, etc.), even though all the available solar observations in a suitable time period were carefully examined. Thus while it is generally true that a major geomagnetic storm is more likely to be driven by a frontside fast halo CME associated with a major flare, our study indicates a broad distribution of source properties. The implications of the results for space weather forecasting are briefly discussed."

---
MARKER : "2007_spie_66890c"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Hick, P.P., Buffington, A., Jackson, B.V."
TITLE  : "A procedure for fitting point sources in SMEI white-light full-sky maps"
EDITOR : "Fineschi, S., Viereck, R.A."
CTITLE : "Solar physics and space weather instrumentation II"
SERIAL : "Proc. SPIE"
VOLUME : "6689"
PAGE   : "66890C, 1-8"
YEAR   : "2007-09"
DOI    : "10.1117/12.734808"
TOPKEY : "Coriolis-SMEI"
ABS    : "The Solar Mass Ejection Imager (SMEI) instrument consists of three CCD cameras with individual fields of view of 60&deg; by 3&deg; that combined sweep a 160&deg; arc of sky. SMEI covers the entire sky in one spacecraft orbit of 102 minutes. Individual 4-s exposures from each orbit are assembled into full-sky maps. The primary objective in the SMEI data reduction is to isolate the Thomson-scattering signal across the sky from free electrons in the solar wind. One of the steps needed to achieve the required photometric precision is the individual fitting and removal of stars brighter than 6th magnitude from the full-sky maps. The point-spread function of the SMEI optics has several unusual properties. It has a full width of about one degree, is asymmetric, and varies in width depending on where in the field of view the image is formed. Moreover, the orientation of the PSF on the sidereal sky rotates over 360&deg; over the course of a year. We describe the procedure used to fit and subtract individual stars from the SMEI full-sky maps. A by-product of this procedure are time series at the orbital time resolution for stars brighter than 6th magnitude. These results are used by Buffington et al. (2007) to calibrate the SMEI instrument against the LASCO C3 coronagraph."

---
MARKER : "2007_spie_66890b"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Buffington, A., Morrill, J.S., Hick, P.P., Howard, R.A., Jackson, B.V., Webb, D.F."
TITLE  : "Analyses of the comparative responses of SMEI and LASCO"
EDITOR : "Fineschi, S., Viereck, R.A."
CTITLE : "Solar physics and space weather instrumentation II"
SERIAL : "Proc. SPIE"
VOLUME : "6689"
PAGE   : "66890B, 1-6"
YEAR   : "2007-09"
DOI    : "10.1117/12.734658"
TOPKEY : "Coriolis-SMEI"
ABS    : "Surface-brightness responses of the SOHO-LASCO C3 coronagraph and of the Solar Mass Ejection Imager (SMEI) are compared, using measurements of a selection of bright stars that have been observed in both instruments. Seventeen stars are selected that are brighter than 4.5 magnitudes, are not known variables, and do not have a neighboring bright star. Comparing observations of these determines a scaling relationship between surface-brightness measurements from one instrument to those from the other. We discuss units of surface brightness for the two instruments, and estimate a residual uncertainty for the present scaling relationship."

---
MARKER : "2007_spie_668911"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Bisi, M.M., Jackson, B.V., Fallows, R.A., Breen, A.R., Hick, P.P., Wannberg, G., Thomasson, P., Jordan, C., Dorrian, G.D."
TITLE  : "Combined STELab, EISCAT, ESR, and MERLIN IPS observations of the solar wind"
EDITOR : "Fineschi, S., Viereck, R.A."
CTITLE : "Solar physics and space weather instrumentation II"
SERIAL : "Proc. SPIE"
VOLUME : "6689"
PAGE   : "668911, 1-10"
YEAR   : "2007-09"
DOI    : "10.1117/12.735443"
TOPKEY : "IPS"
ABS    : "The technique of interplanetary scintillation (IPS) can be used to probe interplanetary space between the Sun and Earth most-commonly in terms of speed and also by using the scintillation-level (g-level) as a proxy for density. We combine the large spatial-scale 3D tomographic techniques previously only applied to IPS data from the Solar Terrestrial Environment Laboratory (STELab) array, Nagoya University in Japan, and the previously operational Cambridge IPS system in England, with the finer-scale capabilities of the longer baselines between the systems of the Multi-Element Radio-Linked Interferometer Network (MERLIN) in the UK, and the European Incoherent SCATter (EISCAT) radar and the EISCAT Svalbard Radar (ESR) in northern Scandinavia. Using the UCSD 3D reconstruction technique, we present results of detailed measurements of speed in the solar wind and also those of solar wind flow-directions, constrained by the large-scale density tomography through the use of a kinematic model, as well as applying this tomographic technique for the first time to the MERLIN, EISCAT, and ESR IPS solar wind speed observations in terms of velocity."

---
MARKER : "2007_spie_66890g"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Hick, P.P., Buffington, A., Bisi, M.M., Jensen, E.A."
TITLE  : "SMEI observations in the STEREO era"
EDITOR : "Fineschi, S., Viereck, R.A."
CTITLE : "Solar physics and space weather instrumentation II"
SERIAL : "Proc. SPIE"
VOLUME : "6689"
PAGE   : "66890G, 1-14"
YEAR   : "2007-09"
DOI    : "10.1117/12.734870"
TOPKEY : "Coriolis-SMEI"
ABS    : "White-light Thomson scattering observations from the Solar Mass Ejection Imager (SMEI) have recorded the inner heliospheric response to many CMEs. Some of these are also observed from the LASCO instrumentation and, most recently, the STEREO spacecraft. Here, we detail several CME events in SMEI observations that have also been observed by the LASCO instrumentation and STEREO spacecrafts. We show how SMEI is able to measure CME events from their first observations as close as 20&deg; from the solar disk until they fade away in the SMEI 180&deg; field of view. We employ a 3D reconstruction technique that provides perspective views as observed from Earth, from outward-flowing solar wind. This is accomplished by iteratively fitting the parameters of a kinematic solar wind density model to the SMEI white-light observations and, where possible, including interplanetary scintillation (IPS) velocity data. This 3D modeling technique enables separating the true heliospheric response in SMEI from background noise, and reconstructing the 3D heliospheric structure as a function of time. These reconstructions allow both separation of CME structure from other nearby heliospheric features and a determination of CME mass. Comparisons with LASCO and STEREO images for individual CMEs or portions of them allow a detailed view of changes to the CME shape and mass as they propagate outward."

---
MARKER : "2007_jgr_112_a09103"
TYPE   : "in_journal "
AUTHOR : "Kahler, S.W., Webb, D.F."
TITLE  : "V arc interplanetary coronal mass ejections observed with the Solar Mass Ejection Imager"
SERIAL : "J. Geophys. Res."
VOLUME : "112"
PAGE   : "A09103"
YEAR   : "2007-09"
DOI    : "10.1029/2007JA012358"
TOPKEY : "Coriolis-SMEI"
ABS    : "Since February 2003, the Solar Mass Ejection Imager (SMEI) has been observing interplanetary coronal mass ejections (ICMEs) at solar elongation angles &epsilon; &gt; 20&deg;. The ICMEs generally appear as loops or arcs in the sky, but five show distinct outward concave shapes that we call V arcs. We expect to observe some V arcs, formed by trailing edges of ICME flux ropes or by leading ICME edges sheared by solar wind (SW) speed gradients at the heliospheric current sheet. We characterize the properties of these V arcs and compare them with average properties of all SMEI ICMEs. The typical V arc speeds argue against a slow MHD shock interpretation for their structures. We estimate the V arc solar source locations and their opening angle dynamics as tests for SW shearing. The first test contradicts but the second supports the SW shearing explanation. The implications of the small number of V arcs observed with SMEI is considered. The point P approximation used to determine the V arc locations and inferred solar source regions is critically examined in Appendix A."

---
MARKER : "2007_apj_667_610"
TYPE   : "in_journal "
AUTHOR : "Howard, T.A., Fry, C.D., Johnston, J.C., Webb, D.F."
TITLE  : "On the evolution of coronal mass ejections in the interplanetary medium"
SERIAL : "Astrophys. J."
VOLUME : "667"
PAGE   : "610-625"
YEAR   : "2007-09"
DOI    : "10.1086/519758"
TOPKEY : "Coriolis-SMEI"
ABS    : "Two coronal mass ejections (CMEs) are presented which were tracked through the LASCO field of view (FOV) within 30 Rsun and later as interplanetary CMEs (ICMEs) through the SMEI FOV from 80 to 150 Rsun. They were also associated with erupting filaments observed by EIT, providing information on trajectory of propagation. This allowed three-dimensional reconstructions of CME/ICME geometry, along with corrected (not sky plane projected) measurements of distance-time (DT) plots for each event to ~0.5 AU. An investigation of morphology was conducted. The results suggest that fine structures of the CMEs are eroded by the solar wind, and curvature becomes more sharply convex outward, suggesting that ICME footpoints remain fixed to the Sun even at 0.5 AU. We also present two models describing the evolution of CMEs/ICMEs at large distances from the Sun (far from the launch mechanism and effects of gravity and solar pressure) and consider two drag models: aerodynamic drag and snowplow. There was little difference between these, and their DT profiles matched well with the SMEI data for event 1. Event 2 showed a net acceleration between the LASCO and SMEI FOVs and we could match the data for this event well by introducing a driving Lorentz force. ICME mass almost doubled as a result of swept-up solar wind material from the snowplow model. Finally, we compared the geometry and kinematics of the ICME with that produced by the HAFv2 model and found that the model reasonably matched the geometry, but overestimated the ICME speed."

---
MARKER : "2007_spie_668910"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jensen, E.A., Russel, C.T."
TITLE  : "Measuring the plane of polarization in a strongly circular signal"
EDITOR : "Fineschi, S., Viereck, R.A."
CTITLE : "Solar Physics and Space Weather Instrumentation II"
SERIAL : "Proc. SPIE"
VOLUME : "6689"
PAGE   : "668910, 1-7"
YEAR   : "2007-09"
DOI    : "10.1117/12.734860"
TOPKEY : "Faraday rotation"
ABS    : "The Cassini spacecraft launched in 1997 on a seven year trans-solar system trajectory to reach and orbit Saturn communicates with a circularly polarized carrier signal at multiple frequencies. The transmitted signal includes a very weak component in the opposite polarization (1%). The plane of polarization of this elliptically polarized signal can be used when Cassini is in superior conjunction with the sun to probe the magnetic field of the solar corona through the process known as Faraday rotation. Using a dual circularly polarized receiver, the two components (Left- and Right-Circularly Polarized) were measured during the Cassini superior conjunction in 2002 and analyzed to determine the plane of polarization. The measured plane of polarization was then corrected for leakage between the two circular components in the polarizer. We discuss the methods used for determining the plane of polarization and calibration of the polarizer."

---
MARKER : "2007_dynamic_sun_237"
TYPE   : "in_book"
AUTHOR : "Svestka, Z."
TITLE  : "Solar activity"
EDITOR : "Dwivedi, B.N."
CTITLE : "Dynamic Sun"
CHAPTER: "13"
PAGE   : "238-261"
YEAR   : "2007-09"
TOPKEY : "solar activity"
PUBLISH: "Cambridge UP"
URL    : "http://www.cambridge.org/us/academic/subjects/astronomy/astrophysics/dynamic-sun"

---
MARKER : "2007_mnrasl_382_l48"
TYPE   : "in_journal "
AUTHOR : "Tarrant, N.J., Chaplin, W.J., Elsworth, Y., Spreckley, S.A., Stevens, I.R."
TITLE  : "Asteroseismology of red giants: photometric observations of Arcturus by SMEI"
SERIAL : "Mon. Not. R. Astron. Soc. Lett."
VOLUME : "382 (1)"
PAGE   : "L48"
YEAR   : "2007-08"
DOI    : "10.1111/j.1745-3933.2007.00387.x"
TOPKEY : "Coriolis-SMEI"
ABS    : "We present new results on oscillations of the K1.5 III giant Arcturus (&alpha; Boo), from analysis of just over 2.5 yr of precise photometric observations made by the Solar Mass Ejection Imager on board the Coriolis satellite. A strong mode of oscillation is uncovered by the analysis, having frequency 3.51&plusmn;0.03 &mu;Hz. By fitting its mode peak, we are able to offer a highly constrained direct estimate of the damping time (&tau; = 24 &plusmn; 1 d). The data also hint at the possible presence of several radial-mode overtones, and maybe some non-radial modes. We are also able to measure the properties of the granulation on the star, with the characteristic time-scale for the granulation estimated to be ~0.50 &plusmn; 0.05 d."

---
MARKER : "2007_solar_phys_244_95"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Harra, L.K., Crooker, N.U., Mandrini, C.H., van Driel-Gesztelyi, L., Dasso, S., Wang, J., Elliott, H., Attril, G., Jackson, B.V., Bisi, M.M."
TITLE  : "How does large flaring activity from the same magnetic field configuration produce oppositely directed magnetic clouds?"
SERIAL : "Solar Phys."
VOLUME : "244 (1/2)"
PAGE   : "95-114"
YEAR   : "2007-08"
DOI    : "10.1007/s11207-007-9002-x"
TOPKEY : "magnetic cloud"
ABS    : "We describe the interplanetary coronal mass ejections (ICMEs) that occurred as a result of a series of solar flares and eruptions from 4 to 8 November 2004. Two ICMEs/magnetic clouds occurring from these events had opposite magnetic orientations. This was despite the fact that the major flares related to these events occurred within the same active region that maintained the same magnetic configuration. The solar events include a wide array of activities: flares, trans-equatorial coronal loop disappearance and reformation, trans-equatorial filament eruption, and coronal hole interaction. The first major ICME/magnetic cloud was predominantly related to the active region 10696 eruption. The second major ICME/magnetic cloud was found to be consistent with the magnetic orientation of an erupting trans-equatorial filament or else a rotation of 160&deg; of a flux rope in the active region. We discuss these possibilities and emphasize the importance of understanding the magnetic evolution of the solar source region before we can begin to predict geoeffective events with any accuracy."

---
MARKER : "2007_jgr_112_a08107"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jones, R.A., Canals, A., Breen, A.R., Fallows, R.A., Bisi, M.M., Lawrence, G."
TITLE  : "Interaction between coronal mass ejections and the solar wind"
SERIAL : "J. Geophys. Res."
VOLUME : "112"
PAGE   : "A08107"
YEAR   : "2007-08"
DOI    : "10.1029/2006JA011875"
TOPKEY : "solar wind, coronal mass ejections"
ABS    : "Observations suggest that the interplanetary extensions of coronal mass ejections (iCMEs) may be accelerated or decelerated in their passage through the solar wind. Interplanetary scintillation measurements (IPS) can detect the passage of iCMEs beyond the field of view of the Large-Angle and Spectrometric Coronagraph coronagraphs and can provide information on their velocities. The European Incoherent Scatter Radar and the Multi Element Radio Linked Interferometer Network systems, with a field of view covering 10-120 solar radii, can provide information on iCMEs in the inner regions of the solar wind. IPS observations can also provide solar wind velocity measurements ahead of the iCME, and using this information, we consider the velocity profile of a number of clearly defined iCMEs and the relationship between iCME velocities and that of the background solar wind. The results provide additional confirmation that iCMEs converge toward the velocity of the solar wind ahead of the event and that most of the resulting acceleration or deceleration occurs in the innermost regions of the solar wind."

---
MARKER : "2007_jgr_112_a06101"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Bisi, M.M., Fallows, A.R., Breen, R.A., Habbal, S.R., Jones, R.A."
TITLE  : "Large-scale structure of the fast solar wind"
SERIAL : "J. Geophys. Res."
VOLUME : "112 (A6)"
PAGE   : "A06101"
YEAR   : "2007-06"
DOI    : "10.1029/2006JA012166"
TOPKEY : "solar wind"
ABS    : "We present the results of a comprehensive study of the fast solar wind near solar minimum conditions using interplanetary scintillation (IPS) data taken with the EISCAT system in northern Scandinavia, and a recent extremely long baseline observation using both EISCAT and MERLIN systems. The results from IPS observations suggest that the fast wind inside 100 solar radii (Rsun) can be represented by a two-mode model in some cases but this distinction is much less clear by in situ distances beyond 1 astronomical unit (215 Rsun). Two distinct fast streams are seen in the extremely long baseline IPS observation; comparison of the IPS line of sight with a synoptic map of white light indicates the faster mode overlies the polar crown and the slower fast mode overlies an equatorial extension of the polar coronal hole."

---
MARKER : "2007_jgr_112_a05106"
TYPE   : "in_journal "
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Tokumaru, M., Kojima, M., Fujiki, K., Yamashita, M., Jackson, B.V."
TITLE  : "The source and propagation of the interplanetary disturbance associated with the full-halo coronal mass ejection on 28 October 2003"
SERIAL : "J. Geophys. Res."
VOLUME : "112"
PAGE   : "A05106"
YEAR   : "2007-05"
DOI    : "10.1029/2006JA012043"
TOPKEY : "Coriolis-SMEI"
ABS    : "Observations of interplanetary scintillations made with the 327-MHz four-station system of the Solar-Terrestrial Environment Laboratory of Nagoya University were analyzed to study the three-dimensional properties of a transient solar wind stream associated with the 28 October 2003 full-halo coronal mass ejection (CME). A loop-shaped high-density regionregion propagating at a significantly slower speed than the CME-driven shock was identified. This feature appeared approximately the same as the structure seen in white-light observations made simultaneously. The orientation of the loop structure was found in general agreement with the inclination of the magnetic flux rope observed at 1 AU. Therefore we propose that the origin of this loop structure included the high-density plasma ejected from the corona in association with the 28 October 2003 CME. By comparing this loop structure with solar wind speed data, we find that the loop structure had a solar source aligned with a slow-speed solar wind regionregion."

---
MARKER : "2007_solar_phys_241_385"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Boyer, J.A., Hick, P.P., Buffington, A., Bisi, M.M., Crider, D.H."
TITLE  : "Analysis of solar wind events using interplanetary scintillation (IPS) remote sensing 3D reconstructions and their comparison at Mars"
SERIAL : "Solar Phys."
VOLUME : "241 (2)"
PAGE   : "385-396"
YEAR   : "2007-04"
DOI    : "10.1007/s11207-007-0276-9"
TOPKEY : "IPS"
ABS    : "Interplanetary Scintillation (IPS) allows observation of the inner heliospheric response to corotating solar structures and coronal mass ejections (CMEs) in scintillation level and velocity. With colleagues at STELab, Nagoya University, Japan, we have developed near-real-time access of STELab IPS data for use in space-weather forecasting. We use a 3D reconstruction technique that produces perspective views from solar corotating plasma and outward-flowing solar wind as observed from Earth by iteratively fitting a kinematic solar wind model to IPS observations. This 3D modeling technique permits reconstruction of the density and velocity structure of CMEs and other interplanetary transients at a relatively coarse resolution: a solar rotational cadence and 10&deg; latitudinal and longitudinal resolution for the corotational model and a one-day cadence and 20&deg; latitudinal and longitudinal heliographic resolution for the time-dependent model. This technique is used to determine solar-wind pressure ('ram' pressure) at Mars. Results are compared with ram-pressure observations derived from Mars Global Surveyor magnetometer data (Crider et al. 2003, J. Geophys. Res. 108(A12), 1461) for the years 1999 through 2004. We identified 47 independent in situ pressure-pulse events above 3.5 nPa in the Mars Global Surveyor data in this time period where sufficient IPS data were available. We detail the large pressure pulse observed at Mars in association with a CME that erupted from the Sun on 27 May 2003, which was a halo CME as viewed from Earth. We also detail the response of a series of West-limb CME events and compare their response observed at Mars about 160&deg; west of the Sun Earth line by the Mars Global Surveyor with the response derived from the IPS 3D reconstructions."

---
MARKER : "2007_jastp_69_109"
TYPE   : "in_journal "
AUTHOR : "Fry, C.D., Detman, T.R., Dryer, M., Smith, Z., Sun, W., Deehr, C.S., Akasofu, S.-I., Wu, C.-C., McKenna-Lawlor, S."
TITLE  : "Real-time solar wind forecasting: Capabilities and challenges"
SERIAL : "J. Atmos. Solar Terr. Phys."
VOLUME : "69"
PAGE   : "109-115"
YEAR   : "2007-02"
DOI    : "10.1016/j.jastp.2006.07.024"
TOPKEY : "Coriolis-SMEI"
ABS    : "A user-friendly, real-time, observation-driven system for forecasting solar wind and interplanetary magnetic field conditions is described. The forecast system presently uses the Hakamada-Akasofu-Fry (version 2) kinematic solar wind model to predict, in real-time, solar wind conditions in the heliosphere, including at the location of Mars, and beyond. Properly characterizing and predicting this region of the space environment are essential steps towards improving the accuracy of 'downstream' space weather models used to forecast the space radiation environment and geomagnetic activity. Representative modeling results are presented and the conclusion is made that uncertainty in determining the physical parameters needed for model inputs from real-time solar observations is the biggest factor limiting the accuracy of solar wind models used for space weather analysis and prediction. Future directions include extending the forecast system via a hybrid approach to include 3D MHD modeling."

---
MARKER : "2006_jgr_111_a12101"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Webb, D.F., Mizuno, D.R., Buffington, A., Cooke, M.P., Eyles, C.J., Fry, C.D., Gentile, L.C., Hick, P.P., Holladay, P.E., Howard, T.A., Hewitt, J.G., Jackson, B.V., Johnston, J.C., Kuchar, T.A.,Mozer, J.B., Price, S., Radick, R.R., Simnett, G.M., Tappin, S.J."
TITLE  : "Solar Mass Ejection Imager (SMEI) observations of coronal mass ejections (CMEs) in the heliosphere"
SERIAL : "J. Geophys. Res."
VOLUME : "111"
PAGE   : "A12101"
YEAR   : "2006-12"
DOI    : "10.1029/2006JA011655"
TOPKEY : "Coriolis-SMEI, coronal mass ejections"
ABS    : "The Solar Mass Ejection Imager (SMEI) on the Coriolis spacecraft has been obtaining white light images of nearly the full sky every 102 minutes for three years. We present statistical results of analysis of the SMEI observations of coronal mass ejections (CMEs) traveling through the inner heliosphere; 139 CMEs were observed during the first 1.5 years of operations. At least 30 of these CMEs were observed by SMEI to propagate out to 1 AU and beyond and were associated with major geomagnetic storms at Earth. Most of these were observed as frontside halo events by the SOHO LASCO coronagraphs."

---
MARKER : "2006_aa_456_651"
TYPE   : "in_journal "
AUTHOR : "Bruntt, H., Southworth, J., Torres, G., Penny, A., Clausen, J.V., Buzasi, D.L."
TITLE  : "Eclipsing binaries observed with the WIRE satellite, I. Discovery and photometric analysis of the new bright A0IV eclipsing binary &Psi; Centauri"
SERIAL : "Astron. Astrophys."
VOLUME : "456"
PAGE   : "651-658"
YEAR   : "2006-09"
DOI    : "10.1051/0004-6361:20065628"
TOPKEY : "Coriolis-SMEI"
ABS    : "Determinations of stellar mass and radius with realistic uncertainties at the level of 1% provide important constraints on models of stellar structure and evolution. We present a high-precision light curve of the A0IV star &Psi; Centauri, from the star tracker on board the WIRE satellite and the Solar Mass Ejection Imager camera on the Coriolis spacecraft. The data show that &Psi; Cen is an eccentric eclipsing binary system with a relatively long orbital period. The WIRE light curve extends over 28.7 nights and contains 41334 observations with 2 mmag point-to-point scatter. The eclipse depths are 0.28 and 0.16 mag, and show that the two eclipsing components of &Psi; Cen have very different radii. As a consequence, the secondary eclipse is total. We find the eccentricity to be e=0.55 with an orbital period of 38.8 days from combining the WIRE light curve with data taken over two years from the Solar Mass Ejection Imager camera. We have fitted the light curve with EBOP and have assessed the uncertainties of the resulting parameters using Monte Carlo simulations. The fractional radii of the stars and the inclination of the orbit have random errors of only 0.1% and 0.01 degrees, respectively, but the systematic uncertainty in these quantities may be somewhat larger. We have used photometric calibrations to estimate the effective temperatures of the components of &Psi; Cen to be 10450&plusmn;300 and 8800&plusmn;300 K, indicating masses of about 3.1 and 2.0 M<sub>sun</sub>. There is evidence in the WIRE light curve for g-mode pulsations in the primary star."

---
MARKER : "2006_aa_456_665"
TYPE   : "in_journal"
AUTHOR : "Kramar, M., Inhester, B., Solanki, S.K."
TITLE  : "Vector tomography for the coronal magnetic field, I. Longitudinal Zeeman effect measurements"
SERIAL : "Astron. Astrophys."
VOLUME : "456"
PAGE   : "665-673"
YEAR   : "2006-09"
DOI    : "10.1051/0004-6361:20064865"
TOPKEY : "magnetic fields, tomography"
ABS    : "Aims. We study the possibility of applying tomographic techniques in order to reconstruct the 3D magnetic field configuration in the solar corona. Our simulations are based on data which can be obtained from longitudinal Zeeman-effect (or from Faraday rotation) measurements obtained during a solar rotation.

Methods. The Zeeman effect provides essentially the integrated line-of-sight component of the magnetic field. The reconstruction problem relates to a family of similar problems termed vector tomography. For inversion of this type problems it is known that the curl-free part of a vector field cannot be reconstructed from the integrated along line-of-sight data. To remove the resulting ambiguity of the reconstruction we include the additional constraint, div B=0$, into the inversion similar to smoothing constraints in Tikhonov regularization problems.

Results. It is shown that Zeeman data obtained from vantage points in the ecliptic plane alone is sensitive only to certain magnetic field structures. For a full reconstruction it is necessary either to have also observations from viewing directions at higher heliographic latitudes, or to combine the longitudinal Zeeman-effect data with observations that provide the transverse component of the field, e.g. from the Hanle effect."

---
MARKER : "2006_apj_642_1216"
TYPE   : "in_journal"
AUTHOR : "Vourlidas, A., Howard, R.A."
TITLE  : "The proper treatment of coronal mass ejection brightness: a new methodology and implications for observations"
SERIAL : "Astrophysical J."
VOLUME : "642 (2)"
PAGE   : "1216-1221"
YEAR   : "2006-05"
DOI    : "10.1086/501122"
TOPKEY : "Thomson scattering, coronal mass ejections"
ABS    : "With the complement of coronagraphs and imagers in the SECCHI suite, we will follow a coronal mass ejection (CME) continuously from the Sun to Earth for the first time. The comparison, however, of the CME emission among the various instruments is not as easy as one might think. This is because the telescopes record the Thomson-scattered emission from the CME plasma, which has a rather sensitive dependence on the geometry between the observer and the scattering material. Here we describe the proper treatment of the Thomson-scattered emission, compare the CME brightness over a large range of elongation angles, and discuss the implications for existing and future white-light coronagraph observations."

---
MARKER : "2006_jgr_111_a04s91"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Buffington, A., Hick, P.P., Wang, X., Webb, D."
TITLE  : "Preliminary three-dimensional analysis of the heliospheric response to the 28 October 2003 CME using SMEI white-light observations"
SERIAL : "J. Geophys. Res."
VOLUME : "111 (A4)"
PAGE   : "A04S91"
YEAR   : "2006-04"
DOI    : "10.1029/2004JA010942"
TOPKEY : "Coriolis-SMEI, coronal mass ejections"
ABS    : "The Solar Mass Ejection Imager (SMEI) has recorded the inner heliospheric response in white-light Thomson scattering to the 28 October 2003 coronal mass ejection (CME). This preliminary report shows the evolution of this particular event in SMEI observations, as we track it from a first measurement at approximately 20&deg; elongation (angular distance) from the solar disk until it fades in the antisolar hemisphere in the SMEI 180&deg; field of view. The large angle and spectrometric coronagraph (LASCO) images show a CME and an underlying bright ejection of coronal material that is associated with an erupting prominence. Both of these are seen by SMEI in the interplanetary medium. We employ a three-dimensional (3-D) reconstruction technique that derives its perspective views from outward flowing solar wind to reveal the shape and extent of the CME. This is accomplished by iteratively fitting the parameters of a kinematic solar wind density model to both SMEI white-light observations and Solar-Terrestrial Environment Laboratory (STELab), interplanetary scintillation (IPS) velocity data. This modeling technique separates the true heliospheric signal in SMEI observations from background noise and reconstructs the 3-D heliospheric structure as a function of time. These reconstructions allow separation of the 28 October CME from other nearby heliospheric structure and a determination of its mass. The present results are the first utilizing this type of 3-D reconstruction with the SMEI data. We determine an excess-over-ambient mass for the southward moving ejecta associated with the prominence material of 7.1&times;10^16 g and a total mass of 8.9&times;10^16 g. Preliminary SMEI white-light calibration indicates that the total mass of this CME including possible associated nearby structures may have been as much as ~2.0&times;10^17 g spread over much of the earthward facing hemisphere."

---
MARKER : "2006_jgr_111_a04105"
TYPE   : "in_journal "
AUTHOR : "Howard, T.A., Webb, D.F., Tappin, S.J., Mizuno, D.R., Johnston, J.C."
TITLE  : "Tracking halo coronal mass ejections from 0 - 1 AU and space weather forecasting using the Solar Mass Ejection Imager (SMEI)"
SERIAL : "J. Geophys. Res."
VOLUME : "111"
PAGE   : "A04105"
YEAR   : "2006-04"
DOI    : "10.1029/2005JA011349"
TOPKEY : "Coriolis-SMEI"
ABS    : "The Solar Mass Ejection Imager (SMEI) has been tracking coronal mass ejections (CMEs) from the Sun to the Earth and beyond since it came online in February 2003. This paper presents some results from the first 19 months of data from SMEI, when over 140 transients of many kinds were observed in SMEI's all-sky cameras. We focus specifically on 20 earthward directed transients, and compare distance-time plots obtained from the SMEI transients with those observed in halo CMEs by Large-Angle Spectrometric Coronograph (LASCO) aboard Solar and Heliospheric Observatory (SOHO), and the arrival time of the shock observed by ACE at 0.99 AU. The geometry of one particular transient is compared using both LASCO and SMEI images in a first attempt to investigate geometry evolution as the transient propagates through the interplanetary medium. For some events, the halo CME, SMEI transient, and shock at 0.99 AU do not match, suggesting that some transients may not correspond to a halo CME. Finally, an evaluation of the potential of SMEI to be used as a predictor of space weather is presented, by comparing the transients observed in SMEI with the 22 geomagnetic storms which occurred during this timeframe. A transient was observed in 14 cases, and distance-time profiles would have allowed a prediction of the arrival time at ACE within 2 hours of its actual arrival for three events, and within 10 hours for eight events. Of these eight events, seven were detected by SMEI more than 1 day before the transient's arrival at the Earth."

---
MARKER : "2006_aa_449_791"
TYPE   : "in_journal"
AUTHOR : "Thompson, W.T."
TITLE  : "Coordinate systems for solar image data"
SERIAL : "Astron. Astrophys"
VOLUME : "449 (2)"
PAGE   : "791-803"
YEAR   : "2006-04"
DOI    : "10.1051/0004-6361:20054262"
TOPKEY : "ephemeris"
ABS    : "A set of formal systems for describing the coordinates of solar image data is proposed. These systems build on current practice in applying coordinates to solar image data. Both heliographic and heliocentric coordinates are discussed. A distinction is also drawn between heliocentric and helioprojective coordinates, where the latter takes the observer's exact geometry into account. The extension of these coordinate systems to observations made from non-terrestial viewpoints is discussed, such as from the upcoming STEREO mission. A formal system for incorporation of these coordinates into FITS files, based on the FITS World Coordinate System, is described, together with examples."

---
MARKER : "2006_iau_s233_347"
TYPE   : "in_proceedings"
AUTHOR : "Johnston, J.C., Webb, D.F., Fry, C.D., Mozer, J.B., Kuchar, T.A., Mizuno, D.R., Howard, T.A."
TITLE  : "Observations of coronal mass ejections from the Solar Mass Ejection Imager and space weather implications"
EDITOR : "Bothmer, V., Hady, A.A."
CTITLE : "Solar Activity and its Magnetic Origin"
SERIAL : "Proc. IAU"
VOLUME : "2"
PAGE   : "347-350"
YEAR   : "2006-03"
PUBLISH: "Cambrige UP"
DOI    : "10.1017/S1743921306002158"
TOPKEY : "Coriolis-SMEI"
ABS    : "The Solar Mass Ejection Imager (SMEI) was launched into a Sun-synchronous orbit in January 2003. Its mission objective is to detect and track coronal mass ejections (CMEs) from the Sun in order to improve space weather forecasts. In the three years since launch, over 200 CMEs, about 30 of which were Earth-directed, have been observed by SMEI. We have been able to track several of these CMEs from the SOHO LASCO coronagraphs (&lt;8&deg; from the Sun) through the SMEI field of view (&gt;20&deg; out to 0.5 AU and beyond, and to observe the morphology and evolution of distinctive features over this wide distance range. We report on comparisons of measurements of CME parameters made in the inner heliosphere with the more typical measurements made nearer the Sun with coronagraphs. We illustrate SMEI's capabilities and present key statistical results on basic CME parameters and the use of SMEI-type data in space weather forecasting models. For example, timely observations by SMEI of CMEs en route to Earth could be input to DoD's operational Hakamada-Akasofu-Fry solar wind model to correct or refine its real-time forecasts of approaching disturbances."

---
MARKER : "2006_apj_637_880"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Buffington, A., Band, D.L., Jackson, B.V., Hick, P.P., Smith, A.C."
TITLE  : "A search for early optical emission at gamma-ray burst locations by the Solar Mass Ejection Imager (SMEI)"
SERIAL : "Astrophys. J."
VOLUME : "637"
PAGE   : "880-888"
YEAR   : "2006-02"
DOI    : "10.1086/498407"
URL    : "http://arxiv.org/abs/astro-ph/0510159"
TOPKEY : "Coriolis-SMEI, gamma rays"
ABS    : "The Solar Mass Ejection Imager (SMEI) views nearly every point on the sky once every 102 minutes and can detect point sources as faint as R~10 mag. Therefore, SMEI can detect or provide upper limits for the optical afterglow from gamma-ray bursts in the tens of minutes after the burst, when different shocked regions may emit optically. Here we provide upper limits for 58 bursts between 2003 February and 2005 April."

---
MARKER : "2006_ilws_goa_071"
TYPE   : "in_proceedings"
AUTHOR : "Webb, D.F., Gopalswamy, N."
TITLE  : "Coronal mass ejections and space weather"
EDITOR : "Gopalswamy, N., Bhattacharyya, A."
CTITLE : "Proc. ILWS Workshop on Solar Influence on the Heliosphere and Earth's Environment: Recent Progress and Prospects"
PAGE   : "71-79"
YEAR   : "2006-02"
TOPKEY : "Coriolis-SMEI"
PLACE  : "Goa, India, 19-24 February 2006"
ABS    : "Coronal mass ejections (CMEs) are a key feature of coronal and interplanetary (IP) dynamics. Major CMEs inject large amounts of mass and magnetic fields into the heliosphere and, when aimed Earthward, can cause major geomagnetic storms and drive IP shocks, a key source of solar energetic particles. Studies over this solar cycle using the excellent data sets from the SOHO, TRACE, Yohkoh, Wind, ACE and other spacecraft and ground-based instruments have improved our knowledge of the origins and early development of CMEs at the Sun and how they affect space weather at Earth. A new heliospheric experiment, the Solar Mass Ejection Imager, has completed 3 years in orbit and has obtained results on the propagation of CMEs through the inner heliosphere and their geoeffectiveness. We review key coronal properties of CMEs, their source regions, their manifestations in the solar wind, and their geoeffectiveness. Halo-like CMEs are of special interest for space weather because they suggest the launch of a geoeffective disturbance toward Earth. However, not all halo CMEs are equally geoeffective and this relationship varies over the solar cycle. Although CMEs are involved with the largest storms at all phases of the cycle, recurrent features such as interaction regions and high speed wind streams can also be geoeffective."

---
MARKER : "2006_solar_phys_233_233"
TYPE   : "in_journal "
AUTHOR : "Tappin, S.J."
TITLE  : "The deceleration of an interplanetary transient from the Sun to 5 AU"
SERIAL : "Solar Phys."
VOLUME : "233"
PAGE   : "233-248"
YEAR   : "2006-02"
DOI    : "10.1007/s11207-006-2065-2"
TOPKEY : "Coriolis-SMEI"
ABS    : "A CME which was first seen in LASCO is tracked through SMEI and on out to Ulysses. These measurements allow us to determine the deceleration and compare different models of the deceleration process. It is found that both a simple 'snow plough' model and an aerodynamic drag model predict a much more rapid deceleration in the lower solar wind than is observed. Therefore some driving force is needed over an extended range of distances to account for the motion of the transient. It is conjectured that at least part of this driving force may be provided by one of two low-latitude coronal holes which were close to the site of the CME."

---
MARKER : "2006_aa_446_747"
TYPE   : "in_journal"
AUTHOR : "Greisen, E.W., Calabretta, M.R., Valdes, F.G., Allen, S.L."
TITLE  : "Representation of spectral coordinates in FITS"
SERIAL : "Astron. Astrophys."
VOLUME : "446 (2)"
PAGE   : "747-771"
YEAR   : "2006-02"
DOI    : "10.1051/0004-6361:20053818"
TOPKEY : "ephemeris"
ABS    : "Greisen and Calabretta (2002, A&amp;A, 395, 1061) describe a generalized method for specifying the coordinates of FITS data samples. Following that general method, Calabretta and Greisen (2002, A&amp;A, 395, 1077) describe detailed conventions for defining celestial coordinates as they are projected onto a two-dimensional plane. The present paper extends the discussion to the spectral coordinates of wavelength, frequency, and velocity. World coordinate functions are defined for spectral axes sampled linearly in wavelength, frequency, or velocity, linearly in the logarithm of wavelength or frequency, as projected by ideal dispersing elements, and as specified by a lookup table."

---
MARKER : "2006_solar_phys_233_1"
TYPE   : "in_journal"
AUTHOR : "Engvold, O., Harvey, J., Leibacher, J., Sakurai, T., Švestka, Z., van Driel-Gesztelyi, L., editors, Solar Physics"
TITLE  : "Editorial Appreciation"
SERIAL : "Solar Phys."
VOLUME : "233 (1)"
PAGE   : "1-2"
YEAR   : "2006-01"
DOI    : "10.1007/s11207-006-2200-0"
REMARK : "editorial"

---
MARKER : "2005_spie_59011b"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Hick, P.P., Buffington, A., Jackson, B.V."
TITLE  : "The SMEI real-time data pipeline: From raw CCD frames to photometrically accurate full-sky maps"
EDITOR : "Fineschi, S., Viereck, R.A."
CTITLE : "Solar physics and space weather instrumentation"
SERIAL : "Proc. SPIE"
VOLUME : "5901"
PAGE   : "59011b, 1-7"
YEAR   : "2005-09"
DOI    : "10.1117/12.617996"
TOPKEY : "Coriolis-SMEI"
ABS    : "The Solar Mass Ejection Imager (SMEI) records a photometric white-light response of the interplanetary medium from Earth orbit over most of the sky. We present the techniques required to process the SMEI data in near real time from the raw CCD images to their final assembly into photometrically accurate maps of the sky brightness of Thomson scattered sunlight. Steps in the SMEI data processing include: integration of new data into the SMEI data base; conditioning to remove from the raw CCD images an electronic offset (pedestal) and a temperature-dependent dark current pattern; placement ('indexing') of the CCD images onto a high-resolution sidereal grid using known spacecraft pointing information. During the indexing the bulk of high-energy-particle hits (cosmic rays), space debris inside the field of view, and pixels with a sudden state change ('flipper pixels') are identified. Once the high-resolution grid is produced, it is reformatted to a lower-resolution set of sidereal maps of sky brightness. From these we remove bright stars, background stars, and a zodiacal cloud model (their brightnesses are retained as additional data products). The final maps can be represented in any convenient sky coordinate system, e.g., Sun-centered Hammer-Aitoff or 'fisheye' projections. Time series at selected sidereal locations are extracted and processed further to remove aurorae, variable stars and other unwanted signals. These time series of the heliospheric Thomson scattering brightness (with a long-term base removed) are used in 3D tomographic reconstructions."

---
MARKER : "2005_spie_59011a"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Yu, Y., Hick, P.P., Jackson, B.V."
TITLE  : "Interactive Visualization of Solar Mass Ejection Imager (SMEI) Volumetric Data"
EDITOR : "Fineschi, S., Viereck, R.A."
CTITLE : "Solar physics and space weather instrumentation"
SERIAL : "Proc. SPIE"
VOLUME : "5901"
PAGE   : "59011a, 1-5"
YEAR   : "2005-09"
DOI    : "10.1117/12.616358"
TOPKEY : "Coriolis-SMEI"
ABS    : "We present a volume rendering system developed for the real time visualization and manipulation of 3D heliospheric volumetric solar wind density and velocity data obtained from the Solar Mass Ejection Imager (SMEI) and interplanetary scintillation (IPS) velocities over the same time period. Our system exploits the capabilities of the VolumePro 1000 board from TeraRecon, Inc., a low-cost 64-bit PCI board capable of rendering up to a 512-cubed array of volume data in real time at up to 30 frames per second on a standard PC. Many volume-rendering operations have been implemented with this system such as stereo/perspective views, animations of time-sequences, and determination of coronal mass ejection (CME) volumes and masses. In these visualizations we highlight one time period where a halo CMEs was observed by SMEI to engulf Earth on October 29, 2003. We demonstrate how this system is used to measure the distribution of structure and provide 3D mass for individual CME features, including the ejecta associated with the large prominence viewed moving to the south of Earth following the late October CME. Comparisons with the IPS velocity volumetric data give pixel by pixel and total kinetic energies for these events."

---
MARKER : "2005_spie_590101"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Buffington, A., Hick, P.P., Wang, X."
TITLE  : "Low resolution three dimensional reconstruction of CMEs using Solar Mass Ejection Imager (SMEI) data"
EDITOR : "Fineschi, S., Viereck, R.A."
CTITLE : "Solar physics and space weather instrumentation"
SERIAL : "Proc. SPIE"
VOLUME : "5901"
PAGE   : "590101, 1-12"
YEAR   : "2005-09"
DOI    : "10.1117/12.616329"
TOPKEY : "Coriolis-SMEI"
ABS    : "White-light Thomson scattering observations from the Solar Mass Ejection Imager (SMEI) have recorded the inner heliospheric response to many CMEs. Here we detail how we determine the extent of several CME events in SMEI observations (including those of 28 May 28 and 28 October, 2003). We show how we are able to measure these events from their first observations as close as 20&deg; from the solar disk until they fade away in the SMEI 180&deg; field of view. We employ a 3D reconstruction technique that provides perspective views from outward-flowing solar wind as observed at Earth. This is accomplished by iteratively fitting the parameters of a kinematic solar wind density model to the SMEI white light observations and to Solar-Terrestrial Environment Laboratory (STELab), interplanetary scintillation (IPS) velocity data. This 3D modeling technique enables separating the true heliospheric response in SMEI from background noise, and reconstructing the 3D heliospheric structure as a function of time. These reconstructions allow both separation of the 28 October CME from other nearby heliospheric structure and a determination of its mass. Comparisons with LASCO for individual CMEs or portions of them allow a detailed view of changes to the CME shape and mass as they propagate outward."

---
MARKER : "2005_sw11_soho16_1"
TYPE   : "in_proceedings"
AUTHOR : "Simnett, G.M."
TITLE  : "CMEs observed by SMEI which are not seen by LASCO"
EDITOR : "Fleck, B., Zurbuchen, T.H., Lacoste, H."
CTITLE : "Proc. Solar Wind 11/SOHO 16: Connecting Sun and Heliosphere"
SERIAL : "ESA SP"
VOLUME : "592"
PAGE   : "767"
YEAR   : "2005-09"
PUBLISH: "ESTEC, Noordwijk, The Netherlands"
TOPKEY : "Coriolis-SMEI"
PLACE  : "Whistler, Canada, 12-17 June 2005"
ABS    : "The Solar Mass Ejection Imager (SMEI) has been observing CMEs in the interplanetary medium since its launch on the Coriolis spacecraft on 6 January 2003. Approximately 1/8<sup>th</sup> of the events which are readily detected in the all-sky images produced once/orbit (102 minutes) are not accompanied by an event visible in LASCO running difference images within 12 hours of the nominal time the event left the Sun. The latter is based on a back-extrapolation of the elongation-time plot of the SMEI event. A further constraint is that the search of the LASCO data was restricted to a position angle within &plusmn; 60&deg; of the position angle of the SMEI event. A further 1/8<sup>th</sup> of the SMEI events were accompanied by extremely faint LASCO events, which would not have been detected by a casual observer, but which otherwise matched well with the SMEI elongation-time plot at the same position angle. The conclusion form this work is that erupting magnetic structures from the Sun must frequently accumulate mass as they travel through the interplanetary medium."

---
MARKER : "2005_jgr_110_a09s14"
TYPE   : "in_journal "
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Reiner, M.J., Jackson, B.V., Webb, D.F., Mizuno, D.R., Kaiser, M.L., Bougeret, J.-L."
TITLE  : "CME kinematics deduced from white-light (SMEI) and radio (Wind/WAVES) observations"
SERIAL : "J. Geophys. Res."
VOLUME : "110 (A9)"
PAGE   : "A09S14"
YEAR   : "2005-09"
DOI    : "10.1029/2004JA010943"
TOPKEY : "Coriolis-SMEI"
ABS    : "White-light and radio observations are combined to deduce the coronal and interplanetary kinematics of a fast coronal mass ejection (CME) that was ejected from the Sun at about 1700 UT on 2 November 2003. The CME, which was associated with an X8.3 solar flare from W56&deg;, was observed by the Mauna Loa and Solar and Heliospheric Observatory (SOHO) Large-Angle Spectrometric Coronograph (LASCO) coronagraphs to 14 Rsun. The measured plane-of-sky speed of the LASCO CME was 2600 km s^-1. To deduce the kinematics of this CME, we use the plane-of-sky white light observations from both the Solar Mass Ejection Imager (SMEI) all-sky camera on board the Coriolis spacecraft and the SOHO/LASCO coronagraph, as well as the frequency drift rate of the low-frequency radio data and the results of the radio direction-finding analysis from the WAVES experiment on the Wind spacecraft. In agreement with the in situ observations for this event, we find that both the white light and radio observations indicate that the CME must have decelerated significantly beginning near the Sun and continuing well into the interplanetary medium. More specifically, by requiring self-consistency of all the available remote and in situ data, together with a simple, but not unreasonable, assumption about the general characteristic of the CME deceleration, we were able to deduce the radial speed and distance time profiles for this CME as it propagated from the Sun to 1 AU. The technique presented here, which is applicable to mutual SMEI/WAVES CME events, is expected to provide a more complete description and better quantitative understanding of how CMEs propagate through interplanetary space, as well as how the radio emissions, generated by propagating CME/shocks, relate to the shock and CME. This understanding can potentially lead to more accurate predictions for the onset times of space weather events, such as those that were observed during this unique period of intense solar activity."

---
MARKER : "2005_icrc29_2_267"
TYPE   : "in_proceedings"
AUTHOR : "Kahler, S.W., Simnett, G.M."
TITLE  : "Imaging interplanetary disturbances causing Forbush decreases"
EDITOR : "Sripathi Acharya, B., Gupta, S., Jagadeesan, P., Jain, A., Karthikeyan, S., Morris, S., Tonwar, S."
CTITLE : "Proc. 29^th Intl. Cosmic Ray Conf."
VOLUME : "2"
PAGE   : "267-270"
YEAR   : "2005-08"
TOPKEY : "Coriolis-SMEI"
PLACE  : "Pune, India, 3-10 August 2005"
ABS    : "Forbush decreases (FDs) in neutron monitor (NM) counting rates are caused by enhance magnetic fields in interplanetary shocks and solar ejecta that shield the Earth from galactic cosmic rays (GCRs). The solar origins of those ejecta can be observed as coronal mass ejections (CMEs) in coronagraphs, but their propagation through interplanetary space near of past the Earth has not been previously observable. The Solar Mass Ejection Image (SMEI), launched into polar Earth orbit in January 2003, now allows us to search for the white light signatures of interplanetary CMEs (ICMEs) responsible for FDs. SMEI is unique in that it can monitor the progress of CMEs through the inner heliosphere out to disturbances beyond 1 AU and distinguish those which hit the Earth from those that do not. For comparison with SMEI observations, we selected all FDs of &gt;= 2% observed with the Oulu, Finland, NM. We find an excellent association of SMEI CMEs with those FDs and for each of the associated SMEI CMEs a good candidate associated LASCO CME was also found. The SMEI observations provide information on the approximate spatial locations and trajectories of large ICMEs that may result in FDs and hencee can be useful as a space weather tool."

---
MARKER : "2005_icrc29_1_165"
TYPE   : "in_proceedings"
AUTHOR : "Simnett, G.M., Kahler, S.W."
TITLE  : "Interplanetary CMEs without observed coronagraph CMEs"
EDITOR : "Sripathi Acharya, B., Gupta, S., Jagadeesan, P., Jain, A., Karthikeyan, S., Morris, S., Tonwar, S."
CTITLE : "Proc. 29^th Intl. Cosmic Ray Conf."
VOLUME : "1"
PAGE   : "165-168"
YEAR   : "2005-08"
TOPKEY : "Coriolis-SMEI"
PLACE  : "Pune, India, 3-10 August 2005"
ABS    : "The SMEI has observed 88 interplanetary coronal mass ejections (ICMEs) in 2003. This work has established that most of those ICMEs, observed beyond ~30&deg; elongation angles, are associated with bright CMEs with appropriate speeds and position angles observed out to 30 R<sub>sun</sub> in the SOHO LASCO coronagraph. However, about one quarter of the ICMEs do not have obvious candidate CME associations despite good LASCO observational coverage. We examine the characteristics of those SMEI ICMEs without LASCO CME associations to determine whether or how they differ from the other ICMEs. In particular we examine the speed profiles and brightness of those ICMEs. We discuss possible ways in which the ICMEs can arise as discrete observable structures in the interplanetary medium without being observed to any significant degree in coronagraph images."

---
MARKER : "2005_solar_phys_230_1"
TYPE   : "in_journal"
AUTHOR : "Rottman, G., Woods, T., George, V., Harvey, J., Švestka, Z., Engvold, O."
TITLE  : "Preface topical issue 'The Solar Radiation and Climate Experiment (SORCE): Mission description and early results'"
SERIAL : "Solar Phys."
VOLUME : "230 (1-2)"
PAGE   : "1-2"
YEAR   : "2005-08"
DOI    : "10.1007/s11207-005-1588-2"

---
MARKER : "2005_spie_590118"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Buffington, A., Jackson, B.V., Hick, P.P."
TITLE  : "Space performance of the multistage labyrinthine SMEI baffle"
EDITOR : "Fineschi, S., Viereck, R.A."
CTITLE : "Solar physics and space weather instrumentation"
SERIAL : "Proc. SPIE"
VOLUME : "5901"
PAGE   : "590118, 1-10"
YEAR   : "2005-08"
DOI    : "10.1117/12.615526"
TOPKEY : "Coriolis-SMEI"
ABS    : "The Solar Mass Ejection Imager (SMEI) was launched on 6 January 2003, and shortly thereafter raised to a nearly circular orbit at 840 km. Three SMEI CCD cameras on the zenith-nadir oriented CORIOLIS spacecraft cover most of the sky beyond about 20&deg;. from the Sun, each 102-minute orbit. Data from this instrument provide precision visible-light photometric sky maps. Once starlight and other constant or slowly varying backgrounds are subtracted, the residue is mostly sunlight that has been Thomson-scattered from heliospheric electrons. These maps enable 3-dimensional tomographic reconstruction of heliospheric density and velocity. This analysis requires 0.1% photometry and background-light reduction below one S10 (the brightness equivalent of a 10th magnitude star per square degree). Thus 10-15 of surface-brightness reduction is required relative to the solar disk. The SMEI labyrinthine baffle provides roughly 10^-10 of this reduction; the subsequent optics system provides the remainder. We analyze data obtained over two years in space, and evaluate the full system's stray-light rejection performance."

---
MARKER : "2005_jgr_110_7230"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Mizuno, D.R., Buffington, A., Cooke, M.P., Eyles, C.J., Hick, P.P., Holladay, P.E., Jackson, B.V., Johnston, J.C., Kuchar, T.A., Mozer, J.B., Price, S.D., Radick, R.R., Simnett, G.M., Sinclair, D., Tappin, S.J., Webb, D.F."
TITLE  : "Very high-altitude aurora observations with the Solar Mass Ejection Imager"
SERIAL : "J. Geophys. Res."
VOLUME : "110"
PAGE   : "7230-7247"
YEAR   : "2005-07"
DOI    : "10.1029/2004JA010689"
TOPKEY : "Coriolis-SMEI"
ABS    : "The Solar Mass Ejection Imager (SMEI) is a sensitive scanning instrument mounted on the Coriolis satellite that assembles an approximately all-sky image of the heliosphere in red-biased visible light once per orbit. Its lines of sight pass obliquely through the topside ionosphere and magnetosphere. We present serendipitous observations of a visual phenomenon detected at high altitudes (&gt;840 km) over the auroral zones and polar caps. The phenomenon is observed in two basic forms. The first, and more common, are periods of brief (1-3 min), nearly uniform illumination of the imager's field of view, which we interpret as transits of the satellite through a luminous medium. The second appear as localized filamentary structures, which we interpret as columns of luminous material, viewed from a distance, possibly extending to visible altitudes of 2000 km or higher. More than 1000 occurrences of these phenomena were recorded during the first full year of operations. These observations are well correlated in brightness and frequency with periods of enhanced geomagnetic activity."

---
MARKER : "2005_solar_phys_229_305"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z., Farnik, F."
AFFIL  : "UCSD-CASS-SHPG, CZECH-ONDREJOV"
TITLE  : "Evidence linking slow solar wind streams to long-decay X-ray events"
SERIAL : "Solar Phys."
VOLUME : "229 (2)"
PAGE   : "305-312"
YEAR   : "2005-07"
DOI    : "10.1007/s11207-005-6881-6"
TOPKEY : "solar wind, X-rays"
ABS    : "Outflow of slow solar wind from solar active regions has been reported in recent years by many different authors. Therefore, in this paper we have studied synoptic maps of the solar wind density (SWD) based on interplanetary scintillation (IPS) data for available parts of all the years 1991-1994 and 1997-2001 to verify correlations of maxima in SWD with sources in active regions. We have found convincing evidence that eruptive flares in active regions, and thus X-ray long-decay events (LDEs) in general, can produce short-lived enhancements of the SWD. However, we were not able to get statistically convincing evidence that active regions can be permanent sources of slow solar wind, and propose three possible reasons for this negative result."

---
MARKER : "2005_solar_phys_229_1"
TYPE   : "in_journal"
AUTHOR : "Engvold, O., Harvey, J., Svestka, Z."
TITLE  : "Editorial"
SERIAL : "Solar Phys."
VOLUME : "229 (1)"
PAGE   : "1"
YEAR   : "2005-06"
DOI    : "10.1007/s11207-005-0087-9"
TOPKEY : "solar physics"
REMARK : "editorial"

---
MARKER : "2005_solar_phys_227_339"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Dunn, T., Jackson, B.V., Hick, P.P., Buffington, A., Zhao, X.P."
TITLE  : "Comparative analyses of the CSSS calculation in the UCSD tomographic solar observations"
SERIAL : "Solar Phys."
VOLUME : "227"
PAGE   : "339-353"
YEAR   : "2005-04"
DOI    : "10.1007/s11207-005-2759-x"
TOPKEY : "IPS, solar wind"
ABS    : "We describe a new method to derive the interplanetary magnetic field (IMF) out to 1 AU from photospheric magnetic field measurements. The method uses photospheric magnetograms to calculate a source surface magnetic field at 15Rs. Specifically, we use Wilcox Solar Observatory (WSO) magnetograms as input for the Stanford Current-Sheet Source-Surface (CSSS) model. Beyond the source surface the magnetic field is convected along velocity flow lines derived by a tomographic technique developed at UCSD and applied to interplanetary scintillation (IPS) observations. We compare the results with in situ data smoothed by an 18-h running mean. Radial and tangential magnetic field amplitudes fit well for the 20 Carrington rotations studied, which are largely from the active phase of the solar cycle. We show exemplary results for Carrington rotation 1965, which includes the Bastille Day event."

---
MARKER : "2005_solar_radio_chapt_17"
TYPE   : "in_book"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Hick, P.P."
TITLE  : "Three-dimensional tomography of interplanetary disturbances"
EDITOR : "Gary, D.E., Keller, C.U."
CTITLE : "Solar and space weather radiophysics, current status and future developments"
CHAPTER: "17"
SERIAL : "Astrophysics and Space Science Library"
VOLUME : "314"
PAGE   : "355-386"
PUBLISH: "Kluwer Academic Publ., Dordrecht, The Netherlands"
YEAR   : "2005"
DOI    : "10.1007/1-4020-2814-8_17"
TOPKEY : "IPS, space weather"
ABS    : "We have developed a Computer Assisted Tomography (CAT) program that modifies a three-dimensional kinematic heliospheric model to fit interplanetary scintillation (IPS) or Thomson scattering observations. The tomography program iteratively changes this global model to least-squares fit the data. Both a corotating and time-dependent model can be reconstructed. The short time intervals of the time-dependent modeling (to shorter than 1 day) force the heliospheric reconstructions to depend on outward solar wind motion to give perspective views of each point in space accessible to the observations, allowing reconstruction of interplanetary Coronal Mass Ejections (CMEs) as well as corotating structures. We show these models as velocity or density Carrington maps and remote views. We have studied several events, including the 2000 July 14 Bastille-Day halo CME and several intervals using archival Cambridge IPS data, and we have also used archival Helios photometer data to reproduce the heliosphere. We check our results by comparison with additional remote-sensing observations, and in-situ observations from near-Earth spacecraft. A comparison of these observations and the Earth forecasts possible using them is available in real time on the World Wide Web using IPS data from the Solar Terrestrial Environment Laboratory, Japan."

---
MARKER : "2004_solar_phys_225_177"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Buffington, A., Hick, P.P., Altrock, R.C., Figueroa, S., Holladay, P.E., Johnston, J.C., Kahler, S.W., Mozer, J.B., Price, S., Radick, R.R., Sagalyn, R., Sinclair, D., Simnett, G.M., Eyles, C.J., Cooke, M.P., Tappin, S.J., Kuchar, T., Mizuno, D., Webb, D.F., Anderson, P.A., Keil, S.L., Gold, R.E., Waltham, N.R."
TITLE  : "The Solar Mass Ejection Imager (SMEI) Mission"
SERIAL : "Solar Phys."
VOLUME : "225"
PAGE   : "177-207"
YEAR   : "2004-11"
DOI    : "10.1007/s11207-004-2766-3"
TOPKEY : "Coriolis-SMEI"
ABS    : "We have launched into near-Earth orbit a solar mass-ejection imager (SMEI) that is capable of measuring sunlight Thomson-scattered from heliospheric electrons from elongations to as close as 18&deg; to greater than 90&deg; from the Sun. SMEI is designed to observe time-varying heliospheric brightness of objects such as coronal mass ejections, co-rotating structures and shock waves. The instrument evolved from the heliospheric imaging capability demonstrated by the zodiacal light photometers of the Helios spacecraft. A near-Earth imager can provide up to three days warning of the arrival of a mass ejection from the Sun. In combination with other imaging instruments in deep space, or alone by making some simple assumptions about the outward flow of the solar wind, SMEI can provide a three-dimensional reconstruction of the surrounding heliospheric density structures."

---
MARKER : "2004_iau_s223_499"
TYPE   : "in_proceedings"
AUTHOR : "Webb, D.F."
TITLE  : "Coronal mass ejections and space weather"
EDITOR : "Stepanov, A., Benevolenskaya, E.E., Kosovichev, A.G."
CTITLE : "Multi-Wavelength Investigations of Solar Activity"
SERIAL : "Proc. IAU 2004"
VOLUME : "2004"
PAGE   : "499-508"
YEAR   : "2004-06"
PUBLISH: "Cambridge UP"
DOI    : "10.1017/S1743921304006696"
TOPKEY : "Coriolis-SMEI"
ABS    : "Coronal mass ejections (CMEs) are a key aspect of coronal and interplanetary dynamics. They can inject large amounts of mass and magnetic fields into the heliosphere, causing major geomagnetic storms and interplanetary shocks, a key source of solar energetic particles. Studies over the past decade using the excellent data sets from the SOHO, TRACE, Wind, ACE and other spacecraft and ground-based instruments have improved our knowledge of the origins and early development of CMEs at the Sun and how they affect space weather at Earth. I review some key coronal properties of CMEs, their source regions, their manifestations in the solar wind, and their geoeffectiveness. Halo-like CMEs are of special interest for space weather because they suggest the launch of a geoeffective disturbance toward Earth. However, their correspondence to geomagnetic storms varies over the solar cycle. Although CMEs are involved with the largest storms at all phases of the cycle, recurrent features such as interaction regions and high speed wind streams can also be geoeffective. A new heliospheric experiment, the Solar Mass Ejection Imager, has completed its first year in orbit and I give some early results."

---
MARKER : "2004_space_weather_2_s03008"
TYPE   : "in_journal "
AUTHOR : "Webb, D., Allen, J."
TITLE  : "Spacecraft and ground anomalies related to the October-November 2003 solar activity"
SERIAL : "Space Weather"
VOLUME : "2"
PAGE   : "S03008"
YEAR   : "2004-03"
DOI    : "10.1029/2004SW000075"
TOPKEY : "Coriolis-SMEI"
ABS    : "During two weeks in late October and early November 2003, a series of large solar events led to high levels of energetic particles in geospace and produced overlapping large geomagnetic storms on 28-30 October. These storms caused effects ranging from power grid failures to satellite shutdowns. A Japanese satellite was lost completely, the U. S. Federal Aviation Administration issued their first-ever high radiation dosage alert for high-altitude aircraft, and astronauts in the International Space Station had to retreat into their heavily shielded service module."

---
MARKER : "2004_spie_5171_001"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Hick, P.P., Buffington, A., Gold, R., Simnett, G.M., Eyles, C.J., Cooke, M.P."
TITLE  : "SMEI: Design and development of an Earth-orbiting all-sky coronagraph"
EDITOR : "Fineschi, S., Gummin, M.A."
CTITLE : "Telescopes and instrumentation for solar astrophysics "
SERIAL : "Proc. SPIE"
VOLUME : "5171"
PAGE   : "1-5"
YEAR   : "2004-02"
DOI    : "10.1117/12.513469"
TOPKEY : "Coriolis-SMEI"
ABS    : "The Air Force/NASA Solar Mass Ejection Imager (SMEI) launched January 6, 2003 is now recording whole sky data on each 100-minute orbit. Precise photometric sky maps of the heliosphere around Earth are expected from these data. The SMEI instrument extends the heritage of the HELIOS spacecraft photometer systems that have recorded CMEs and other heliospheric structures from close to the Sun into the anti-solar hemisphere. SMEI rotates once per orbit and views the sky away from Earth using CCD camera technology. To optimize the information derived from this and similar instruments, a tomographic technique has been developed for analyzing remote sensing observations of the heliosphere as observed in Thomson scattering. The technique provides 3-dimensional reconstructions of heliospheric density. The tomography program has been refined to analyze time-dependent phenomena such as evolving corotating heliospheric structures and more discrete events such as coronal mass ejections (CMEs), and this improved analysis is being applied to the SMEI data."

---
MARKER : "2004_spie_5171_006"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Dunn, T., Hick, P.P., Jackson, B.V., Zhao, X."
TITLE  : "Comparative analyses of the CSSS magnetic field calculation in the UCSD tomographic solar wind model with in situ spacecraft observations"
EDITOR : "Fineschi, S., Gummin, M.A."
CTITLE : "Telescopes and instrumentation for solar astrophysics "
SERIAL : "Proc. SPIE"
VOLUME : "5171"
PAGE   : "6-13"
YEAR   : "2004-02"
DOI    : "10.1117/12.513759"
TOPKEY : "remote sensing, solar wind"
ABS    : "Our tomographic techniques developed over the last few years are based on kinematic models of the solar wind. This allows us to determine the large-scale three-dimensional extents of solar wind structures using interplanetary scintillation (IPS) observations and Thomson scattering brightness data in order to forecast their arrival at Earth in real time. We are specifically interested in a technique that can be combined with observations presently available from IPS velocity data and with observations which will become available from the Solar Mass Ejection Imager. In this paper, we introduce magnetic field projections from solar surface magnetogram data using the Stanford Current-Sheet Source Surface model at the source surface of our model and extrapolate the magnetic field out to and beyond Earth. The results are compared with in situ data. Real time projections of these data are available on our web site at: http://cassfos02.ucsd.edu/solar/forecast/index_v_n.html and http://cassfos02.ucsd.edu/solar/forecast/index_br_bt.html"

---
MARKER : "2004_spie_5171_280"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Wang, X., Hick, P.P., Jackson, B.V., Buffington, A., Bailey, M."
TITLE  : "Visualization of remotely-sensed heliospheric plasmas for space weather applications"
EDITOR : "Fineschi, S., Gummin, M.A."
CTITLE : "Telescopes and instrumentation for solar astrophysics "
SERIAL : "Proc. SPIE"
VOLUME : "5171"
PAGE   : "280-286"
YEAR   : "2004-02"
DOI    : "10.1117/12.513117"
TOPKEY : "remote sensing"
ABS    : "We demonstrate a software application designed for the display and interactive manipulation of 3D heliospheric volume data, such as solar wind density, velocity and magnetic field. The Volume Explorer software exploits the capabilities of the Volume Pro 1000 (from TeraRecon, Inc.), a low-cost 64-bit PCI board capable of rendering a 512-cubed array of volume data in real time at up to 30 frames per second on a standard PC. The application allows stereo and perspective views, and animations of time-sequences. We show examples of three-dimensional heliospheric volume data derived from tomographic reconstructions based on heliospheric remote sensing observations of the heliospheric density and velocity structure. Currently these reconstructions are based on archival IPS and Thomson scattering data. In the near future we expect to add reconstructions based on the all-sky observations from the recently launched Solar Mass Ejection Imager."

---
MARKER : "2004_spie_5171_287"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Hick, P.P., Jackson, B.V."
TITLE  : "Heliospheric tomography: an algorithm for the reconstruction of the 3D solar wind from remote sensing observations"
EDITOR : "Fineschi, S., Gummin, M.A."
CTITLE : "Telescopes and instrumentation for solar astrophysics "
SERIAL : "Proc. SPIE"
VOLUME : "5171"
PAGE   : "287-297"
YEAR   : "2004-02"
DOI    : "10.1117/12.513122"
TOPKEY : "remote sensing"
ABS    : "Over the past years we have developed a tomographic technique for using heliospheric remote sensing observations (i.e. interplanetary scintillation and Thomson scattering data) for the reconstruction of the three-dimensional solar wind density and velocity in the inner heliosphere. We describe the basic algorithm on which our technique is based. To highlight the details of the reconstruction algorithm we specifically emphasize the implementation of corotating tomography using IPS g -level and IPS velocity observations as proxies for the solar wind density and velocity, respectively. We provide some insight into the modifications required to expand the technique into a fully time-dependent tomography, and to use Thomson scattering brightness (instead of g -level) as a proxy for the solar wind density."

---
MARKER : "2004_eos_85_2"
TYPE   : "in_journal"
AUTHOR : "Showstack, R."
TITLE  : "Instrument demonstrates ability to closely track coronal mass ejections"
CTITLE : "EOS Trans. AGU"
VOLUME : "85"
PAGE   : "2"
YEAR   : "2004-01"
DOI    : "10.1029/2004EO010004"
TOPKEY : "Coriolis-SMEI"
ABS    : "A proof-of-concept experiment orbiting 840 km above Earth demonstrates the possibility of instituting a real-time, early warning system for coronal mass ejections which can cause large geomagnetic storms on the planet, according to scientists involved with the project.

Whether or not the experimental Solar Mass Ejection Imager, or SMEI, is able to provide such early warnings, it should pave the way for a future mission to do this, according to mission scientists at an 11 December briefing held during the AGU Fall Meeting in San Francisco."

---
MARKER : "2004_grl_31_2802"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Tappin, S.J, Buffington, A., Cooke, M.P., Eyles, C.J., Hick, P.P., Holladay, P.E., Jackson, B.V., Johnston, J.C., Kuchar, T., Mizuno, D., Mozer, J.B., Price, S., Radick, R.R., Simnett, G.M., Sinclair, D., Waltham, N.R., Webb, D.F."
TITLE  : "Tracking a major interplanetary disturbance with SMEI"
SERIAL : "Geophys. Res. Lett."
VOLUME : "31"
PAGE   : "L2802-L2805"
YEAR   : "2004-01"
DOI    : "10.1029/2003GL018766"
TOPKEY : "Coriolis-SMEI"
ABS    : "We present the first clear observations of an Earth-directed interplanetary disturbance tracked by the Solar Mass Ejection Imager (SMEI). We find that this event can be related to two halo CMEs seen at the Sun about 2 days earlier, and which merged in transit to 1 AU. The disturbance was seen about 16 hours before it reached Earth,and caused a severe geomagnetic storm at the time which would have been predicted had SMEI been operating as a real-time monitor. It is concluded that SMEI is capable of giving many hours advance warning of the possible arrival of interplanetary disturbances."

---
MARKER : "2003_solar_phys_218_183"
TYPE   : "in_journal"
AUTHOR : "Farnik, F., Karlicky, M., Svestka, Z."
AFFIL  : "CZECH-ONDREJOV, CZECH-ONDREJOV, {UCSD-CASS-SHPG, SRON-UTRECHT}"
TITLE  : "Hard X-ray pulsations in the initial phase of flares"
SERIAL : "Solar Phys."
VOLUME : "218 (1-2)"
PAGE   : "183-195"
YEAR   : "2003-12"
DOI    : "10.1023/B:SOLA.0000013044.61171.d9"
TOPKEY : "flares, X-rays"
ABS    : "When analyzing light curves of hard X-ray bursts recorded by the Hard X-Ray Spectrometer on board the MTI satellite, we have found three events (all associated with major solar flares, two of them in the same active region) which show pulsations in the very initial phase of the burst. Periods of the pulsations range from 25 to 48 s. We compare them with other observations of pulsations of radio waves and in X-rays and conclude that pulsations of this kind have not been observed before. We mention several possible causes and prefer interactions between current-carrying loops as the most likely interpretation of the observed variations."

---
MARKER : "2003_solar_phys_217_319"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Eyles, C.J., Simnett, G.M., Cooke, M.P., Jackson, B.V., Buffington, A., Hick, P.P., Waltham, N.R., King, J.M., Anderson, P.A., Holladay, P.E."
TITLE  : "The Solar Mass Ejection Imager (SMEI)"
SERIAL : "Solar Phys."
VOLUME : "217"
PAGE   : "319-347"
YEAR   : "2003-11"
DOI    : "10.1023/B:SOLA.0000006903.75671.49"
TOPKEY : "Coriolis-SMEI"
ABS    : "We describe an instrument (SMEI) which has been specifically designed to detect and forecast the arrival of solar mass ejections and other heliospheric structures which are moving towards the Earth. Such events may cause geomagnetic storms, with resulting radiation hazards and disruption to military and commercial communications; damage to Earth-orbiting spacecraft; and also terrestrial effects such as surges in transcontinental power transmission lines. The detectors are sensitive over the optical wave-band, which is measured using CCD cameras. SMEI was launched on 6 January 2003 on the Coriolis spacecraft into a Sun-synchronous polar orbit as part of the US DoD Space Test Programme. The instrument contains three cameras, each with a field of view of 60&deg;&times;3&deg;, which are mounted onto the spacecraft such that they scan most of the sky every 102-min orbit. The sensitivity is such that changes in sky brightness equivalent to a tenth magnitude star in one square degree of sky may be detected. Each camera takes an image every 4 s. The normal telemetry rate is 128 kbits s^-1. In order to extract the emission from a typical large coronal mass ejection, stellar images and the signal from the zodiacal dust cloud must be subtracted. This requires accurate relative photometry to 0.1%. One consequence is that images of stars and the zodiacal cloud will be measured to this photometric accuracy once per orbit. This will enable studies of transient zodiacal cloud phenomena, flare stars, supernovae, comets, and other varying point-like objects."

---
MARKER : "2003_aip_sw10_679_75"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Hick, P.P., Buffington, A., Kojima, M., Tokumaru, M., Fujiki, K., Ohmi, T., Yamashita, M."
TITLE  : "Time-dependent tomography of heliospheric features using interplanetary scintillation (IPS) remote-sensing observations"
EDITOR : "Velli, M., Bruno, R., Malara, F."
CTITLE : "Solar Wind Ten"
SERIAL : "AIP Conf. Proc."
VOLUME : "679"
PAGE   : "75-78"
YEAR   : "2003-09"
DOI    : "10.1063/1.1618545"
TOPKEY : "IPS"
ABS    : "We have developed a Computer Assisted Tomography (CAT) program that modifies a time-dependent three-dimensional kinematic heliospheric model to fit interplanetary scintillation (IPS) observations. The tomography program iteratively changes this global model to least-squares fit IPS data. The short time intervals of the kinematic modeling (~1 day) force the heliospheric reconstructions to depend on outward solar wind motion to give perspective views of each point in space accessible to the observations, allowing reconstruction of interplanetary Coronal Mass Ejections (CMEs) as well as corotating structures. We show these models as velocity or density Carrington maps and remote views. We have studied several events, including the July 14, 2000 Bastille-day halo CME. We check our results by comparison with additional remote-sensing observations, and observations from near-Earth spacecraft."

---
MARKER : "2003_esa_sp_535_823"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Hick, P.P., Buffington, A."
TITLE  : "Time-dependent tomography of heliospheric structures using IPS and Thomson scattering observations"
EDITOR : "Wilson, A."
CTITLE : "Intl Solar Cycle Studies (ISCS) Symp. on Solar variability as an input to the Earth's environment"
SERIAL : "ESA SP"
VOLUME : "535"
PAGE   : "823-833"
PUBLISH: "ESTEC, Noordwijk, The Netherlands"
YEAR   : "2003-06"
TOPKEY : "IPS, remote sensing"
ABS    : "The Air Force/NASA Solar Mass Ejection Imager (SMEI) launched January 6, 2003 is now recording whole sky data on each 100-minute orbit. Precise photometric images of the heliosphere around Earth are expected from these data. To optimize the information available from this and similar instruments, we are developing a tomographic technique for analyzing remote sensing observations of the heliosphere using both interplanetary scintillation (IPS) and Thomson scattering data. The technique provides a three-dimensional reconstruction of heliospheric velocities and densities. We have refined our tomography program to analyze time-dependent phenomena such as evolving corotating heliospheric structures and more discrete events such as coronal mass ejections (CMEs)."

---
MARKER : "2003_spie_4853_490"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Buffington, A., Jackson, B.V., Hick, P.P."
TITLE  : "Calculations for, and laboratory measurements of a multistage labyrinthine baffle for SMEI"
EDITOR : "Keil, S.L., Avakyan, S.V."
CTITLE : "Innovative telescopes and instrumentation for solar astrophysics"
SERIAL : "Proc. SPIE"
VOLUME : "4853"
PAGE   : "490-503"
YEAR   : "2003-02"
DOI    : "10.1117/12.460350"
TOPKEY : "Coriolis-SMEI"
ABS    : "The spaceborne Solar Mass Ejection Imager (SMEI) is scheduled for launch into near-earth orbit (&gt;800 km) in early 2003. Three SMEI CCD cameras on the zenith-oriented CORIOLIS spacecraft cover most of the sky each 100-minute orbit. Data from this instrument will provide precision visible-light photometric maps. Once starlight and other constant or slowly varying backgrounds are subtracted, the residue is mostly sunlight that has Thomson-scattered from heliospheric electrons. These maps will enable 3-dimensional tomographic reconstruction of heliospheric density and velocity. The SMEI design provides three cameras, one of which views to within 18&deg; of the solar disk with a field of view 60&deg; long by 3&deg; wide. Placed end-to-end, three fields of view then cover a nearly 180&deg; long strip that sweeps out the sky over each orbit. The 3-dimensional tomographic analysis requires 0.1% photometry and background-light reduction below one S10 (the brightness equivalent of a 10th magnitude star per square degree). Thus 10^-15 of surface-brightness reduction is required relative to the solar disk. The SMEI labyrinthine baffle provides roughly 10^-10 of this reduction; the subsequent optics provides the remainder. We describe the baffle design and present laboratory measurements of prototypes that confirm performance at this level."

---
MARKER : "2003_spie_4853_504"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Dunn, T., Hick, P.P., Jackson, B.V., Zhao, X."
TITLE  : "Inclusion of the CSSS magnetic field calculation into the UCSD tomographic solar wind model"
EDITOR : "Keil, S.L., Avakyan, S.V."
CTITLE : "Innovative telescopes and instrumentation for solar astrophysics"
SERIAL : "Proc. SPIE"
VOLUME : "4853"
PAGE   : "504-510"
YEAR   : "2003-02"
DOI    : "10.1117/12.460414"
TOPKEY : "remote sensing, solar wind, magnetic fields"
ABS    : "Tomographic techniques developed at UCSD over the last few years incorporate a kinematic model of the solar wind to determine and forecast the large-scale three-dimensional extents of velocity and density using interplanetary scintillation (IPS) observations or Thomson scattering brightness data. In this paper, we introduce magnetic field calculations from the Stanford Current-Sheet Source Surface (CSSS) model into our kinematic model. The CSSS model is used to extrapolate the photospheric magnetic field to a source surface at 15 solar radii (Rs). The UCSD kinematic model convects magnetic field from 15 Rs out to and beyond Earth. We compare the results with in situ data near Earth. The spatial relationship between the heliospheric current sheet and coronal mass ejections (CMEs) is shown in remote views of the inner heliosphere."

---
MARKER : "2003_spie_4853_23"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Hick, P.P., Buffington, A."
TITLE  : "Time-dependent tomography of heliospheric features using the three-dimensional reconstruction techniques developed for the Solar Mass Ejection Imager (SMEI)"
EDITOR : "Keil, S.L., Avakyan, S.V."
CTITLE : "Innovative telescopes and instrumentation for solar astrophysics"
SERIAL : "Proc. SPIE"
VOLUME : "4853"
PAGE   : "23-30"
YEAR   : "2003-02"
DOI    : "10.1117/12.460415"
TOPKEY : "Coriolis-SMEI, remote sensing"
ABS    : "Precise photometric images of the heliosphere are expected from the Air Force/NASA Solar Mass Ejection Imager (SMEI) now scheduled for launch in February 2003, and the all-sky cameras proposed for other NASA missions. To optimize the information available from these instruments, we are developing tomographic techniques for analyzing remote sensing observations of heliospheric density as observed in Thomson scattering (e.g. using the Helios photometer data) for eventual use with SMEI. We have refined the tomography program to enable us to analyze time-dependent phenomena, such as the evolution of corotating heliospheric structures and more discrete events such as coronal mass ejections. Both types of phenomena are discerned in our data, and are reconstructed in three dimensions. We use our tomography technique to study the interaction of these phenomena as they move outward from the Sun for several events that have been studied by multiple spacecraft in situ observations and other techniques."

---
MARKER : "2002_solar_phys_211_345"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Hick, P.P."
TITLE  : "Corotational tomography of heliospheric features using global Thomson scattering data"
SERIAL : "Solar Phys."
VOLUME : "211 (1/2)"
PAGE   : "345-356"
YEAR   : "2002-12"
DOI    : "10.1023/A:1022409530466"
TOPKEY : "remote sensing"
ABS    : "The Air Force/NASA Solar Mass Ejection Imager (SMEI) will provide two-dimensional images of the sky in visible light with high (0.1%) photometric precision, and unprecedented sky coverage and cadence. To optimize the information available from these images they must be interpreted in three dimensions. We have developed a Computer Assisted Tomography (CAT) technique that fits a three-dimensional kinematic heliospheric model to remotely-sensed Thomson scattering observations. This technique is designed specifically to determine the corotating background solar wind component from data provided by instruments like SMEI. Here, we present results from this technique applied to the Helios spacecraft photometer observations. The tomography program iterates to a least-squares solution of observed brightnesses using solar rotation, spacecraft motion and solar wind outflow to provide perspective views of each point in space covered by the observations. The corotational tomography described here is essentially the same as used by Jackson et al. (1998) for the analysis of interplanetary scintillation (IPS) observations. While IPS observations are related indirectly to the solar wind density through an assumed (and uncertain) relationship between small-scale density fluctuations and density, Thomson scattering physics is more straightforward, i.e., the observed brightness depends linearly on the solar wind density everywhere in the heliosphere. Consequently, Thomson scattering tomography can use a more direct density-convergence criterion to match observed Helios photometer brightness to brightness calculated from the model density. The general similarities between results based on IPS and Thomson scattering tomography validate both techniques and confirm that both observe the same type of solar wind structures. We show results for Carrington rotation 1653 near solar minimum. We find that longitudinally segmented dense structures corotate with the Sun and emanate from near the solar equator. We discuss the locations of these dense structures with respect to the heliospheric current sheet and regions of activity on the solar surface."

---
MARKER : "2002_aa_395_1061"
TYPE   : "in_journal"
AUTHOR : "Greisen, E.W., Calabretta, M.R."
TITLE  : "Representations of world coordinates in FITS"
SERIAL : "Astron. Astrophys."
VOLUME : "395 (3)"
PAGE   : "1061-1075"
YEAR   : "2002-12"
DOI    : "10.1051/0004-6361:20021326"
TOPKEY : "ephemeris"
ABS    : "The initial descriptions of the FITS format provided a simplified method for describing the physical coordinate values of the image pixels, but deliberately did not specify any of the detailed conventions required to convey the complexities of actual image coordinates. Building on conventions in wide use within astronomy, this paper proposes general extensions to the original methods for describing the world coordinates of FITS data. In subsequent papers, we apply these general conventions to the methods by which spherical coordinates may be projected onto a two-dimensional plane and to frequency/wavelength/velocity coordinates."

---
MARKER : "2002_aa_395_1077"
TYPE   : "in_journal"
AUTHOR : "Calabretta, M.R., Greisen, E.W."
TITLE  : "Representations of celestial coordinates in FITS"
SERIAL : "Astron. Astrophys."
VOLUME : "395 (3)"
PAGE   : "1077-1122"
YEAR   : "2002-12"
DOI    : "10.1051/0004-6361:20021327"
TOPKEY : "ephemeris"
ABS    : "In Paper I, Greisen and Calabretta (2002) describe a generalized method for assigning physical coordinates to FITS image pixels. This paper implements this method for all spherical map projections likely to be of interest in astronomy. The new methods encompass existing informal FITS spherical coordinate conventions and translations from them are described. Detailed examples of header interpretation and construction are given."

---
MARKER : "2002_solar_phys_210_1"
TYPE   : "in_journal"
AUTHOR : "Lin, R., Dennis, B., Benz, A., Harvey, J., Engvold, O., Svestka, Z."
TITLE  : "Preface topical issue 'The Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) - Mission description and early results'"
SERIAL : "Solar Phys."
VOLUME : "210 (1-2)"
PAGE   : "1"
YEAR   : "2002-11"
DOI    : "10.1007/s11207-004-0827-2"
TOPKEY : "solar physics, RHESSI"

---
MARKER : "2002_ursi_p1637"
TYPE   : "in_proceedings"
AUTHOR : "Hick, P., Jackson, B.V., Buffington, A."
AFFIL  : "UCSD-CASS-SHPG"
TITLE  : "Space weather studies using low-frequency interplanetary scintillation observations"
CTITLE : "Proc. URSI General Assembly"
YEAR   : "2002-08"
TOPKEY : "IPS, space weather"
ABS    : "Plasma disturbances originating on the Sun, such as coronal mass ejections (CMEs), are a major factor in determining 'space weather' in the near-Earth environment. Virtually the only current source of routine observations of these disturbances as they propagate through the interplanetary medium are interplanetary scintillation (IPS) data. We review current work on time-dependent tomographic reconstructions of the heliospheric density and velocity based on currently available IPS remote sensing observations. We discuss the importance of the tomographic analysis of IPS data for an effective space weather forecast system, in particular in connection with the future Low Frequency Array (LOFAR) instrumentation."

---
MARKER : "2002_solar_phys_206_143"
TYPE   : "in_journal"
AUTHOR : "Farnik, F., Svestka, Z."
AFFIL  : "CZECH-ONDREJOV, {UCSD-CASS-SHPG, SRON-UTRECHT}"
TITLE  : "X-ray jets in interconnecting loops"
SERIAL : "Solar Phys."
VOLUME : "206 (1)"
PAGE   : "143-154"
YEAR   : "2002-03"
DOI    : "10.1023/A:1014963812437"
TOPKEY : "solar activity"
ABS    : "We present examples of X-ray jets, observed by the Soft X-ray Telescope on board Yohkoh, which followed trajectories of transequatorial interconnecting loops (TILs). All these TILs were preexisting, seen some time before, but were mostly invisible at the time of the onset of the jet which often made them bright along their total length. With few exceptions, these TIL-associated jets have properties very similar to other jets ejected inside active regions or along open field lines (footpoints in X-ray bright points, recurrence, strong collimation, average speed close to 350 km s^-1), but may reach larger lengths, in our examples up to 450,000 km. Exceptions are one jet that moved slower and one that had no brightened area at its supposed source region at the time of its origin (an X-ray bright point appeared there only 3 hours later). It appears that quite a high number of X-ray jets may be of this TIL-associated kind."

---
MARKER : "2002_eos_83_33"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Webb, D.F., Johnston, J.C., Radick, R.R., Team, the SMEI "
TITLE  : "The Solar Mass Ejection Imager (SMEI): A new tool for space weather"
CTITLE : "EOS Trans. AGU"
VOLUME : "83 (4)"
PAGE   : "33"
YEAR   : "2002-01"
DOI    : "10.1029/2002EO000023"
TOPKEY : "Coriolis-SMEI"
ABS    : "Later this year, the U.S. Air Force will launch the Solar Mass Ejection Imager (SMEI). SMEI is an instrument that will detect and measure coronal mass ejections (CMEs) which can cause large geomagnetic storms, a major component of space weather. CMEs are very large structures containing plasma and magnetic fields that are expelled from the Sun into the heliosphere at speeds of several hundred to over 1000 km s^-1. CMEs often drive interplanetary shock waves which, upon arrival at Earth, can cause geomagnetic disturbances. There is currently no reliable way to accurately predict arrival of these disturbances at Earth or to study them in the inner heliosphere. SMEI is designed to fill this gap by detecting and tracking CMEs in interplanetary space before they reach Earth. SMEI data will be complementary to many other satellite missions and national programs, such as the current National Space Weather and International Solar Terrestrial Programs."

---
MARKER : "2002_cospar_coll_ser_12_55"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Kojima, M., Fujiki, K., Tokumaru, M., Ohmi, T., Shimizu, Y., Yokobe, A., Jackson, B.V., Hick, P.L."
TITLE  : "Tomographic analysis of solar wind structure using interplanetary scintillation"
EDITOR : "Lyu, L.-H."
CTITLE : "Space weather study using multi-point techniques "
SERIAL  : "COSPAR Colloquia Series"
VOLUME : "12"
PAGE   : "55-59"
YEAR   : "2002"
TOPKEY : "IPS, space weather"
ABS    : "For space weather research it is important to know the quiet solar wind structure existing as background for transient interplanetary phenomena. Once we know the quiet background structure, transient phenomena are easily recognized as soon as they appear in interplanetary space. The background structure is also important to understand how interplanetary disturbances propagate in it and interact with it. Interplanetary scintillation (IPS) observations have several advantages over in situ spacecraft observations for solar wind studies. Although IPS measurements are biased by the effects of line-of-sight integration, they provide global information about the solar wind. To obtain unbiased solar wind parameters we have developed a computer assisted tomography (CAT) technique. The CAT analysis can retrieve not only unbiased solar wind parameters but also porvide high spatial resolution. We introduce the IPS CAT analysis and discuss its reliabitlity by comparing with Ulysses observations. we also introduce the real-time space weather forecast project currently carried out by UCSD/CASS and STELab under a US-Japan cooperative project."

---
MARKER : "2002_cospar_coll_ser_13_81"
TYPE   : "in_proceedings"
AUTHOR : "Farnik, F., Svestka, Z."
AFFIL  : "CZECH-ONDREJOV, {UCSD-CASS-SHPG, SRON-UTRECHT}"
TITLE  : "X-ray jets in interconnecting loops"
EDITOR : "Martens, P.C.H., Cauffman, D."
CTITLE : "Proc. Multi-Wavelength Observations of Coronal Structure and Dynamics - Yohkoh 10^th Anniversary Meeting"
PLACE  : "Kailua-Kona, HI, USA, 17-20 September 2001"
PAGE   : "81-82"
YEAR   : "2002-00"
DOI    : "10.1016/S0964-2749(02)80018-X"
PUBLISH: "Elsevier Science"
TOPKEY : "solar physics"
ABS    : "We present examples of X-ray jets, observed by Yohkoh/SXT, that followed trajectories of transequatorial interconnecting loops (TILs). All these TILs were preexisting, but mostly invisible at the time of the onset of the jet that often made them bright along their total length. Most of these TIL-associated jets have properties very similar to those of other jets ejected inside active regions or along open field lines (properties such as footpoints in X-ray bright points, recurrence, strong collimation, and average speeds close to 350 km s^-1). However, they may reach larger lengths, up to 450,000 km. Quite a high number of X-ray jets may be of this TIL-associated kind."

---
MARKER : "2001_spie_4498_84"
TYPE   : "in_proceedings"
AUTHOR : "Radick, R.R."
TITLE  : "Solar Mass Ejection Imager (SMEI) space experiment"
EDITOR : "Siegmund, O.H.W., Fineschi, S., Gummin, M.A."
CTITLE : "UV/EUV and Visible Space Instrumentation for Astronomy and Solar Physics"
SERIAL : "Proc. SPIE"
VOLUME : "4498"
PAGE   : "84-90"
YEAR   : "2001-12"
DOI    : "10.1117/12.450048"
TOPKEY : "Coriolis-SMEI"
ABS    : "The Solar Mass Ejection Imager (SMEI) is a proof-of-concept space experiment designed to observe solar coronal mass ejections (CMEs) and forecast their arrival at Earth. SMEI will image CMEs by sensing sunlight scattered from the free electrons in these ejecta (i.e., Thomson scattering). SMEI will be launched by a Titan II rocket into a circular, 830-km, sun-synchronous orbit in mid-2002 as part of the Space Test Program's CORIOLIS mission. SMEI will image nearly the entire sky once per spacecraft orbit over a mission lifetime of three years. Successful operation of SMEI will represent a major step in improving space weather forecasts by providing one- to three-day predictions of geomagnetic storms at the Earth. The SMEI experiment is being designed and constructed by a team of scientists and engineers from the Air Force Research Laboratory, the University of Birmingham (UB) in the United Kingdom, the University of California at San Diego (UCSD), and Boston University. The Air Force, NASA, and UB are providing financial support."

---
MARKER : "2001_jgr_106_20509"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Killen, R.M., Potter, A.E., Reiff, P., Sarantos, M., Jackson, B.V., Hick, P., Giles, B."
TITLE  : "Evidence of space weather at Mercury"
SERIAL : "J. Geophys. Res."
VOLUME : "106"
PAGE   : "20509-20525"
YEAR   : "2001-09"
DOI    : "10.1029/2000JE001401"
TOPKEY : "space weather"
ABS    : "Mercury's sodium atmosphere is known to be highly variable both temporally and spatially. During a week-long period from November 13 to 20, 1997, the total sodium content of the Hermean atmosphere increased by a factor of 3, and the distribution varied daily. We demonstrate a mechanism whereby these rapid variations could be due to solar wind-magnetosphere interactions. We assume that photon-stimulated desorption and meteroritic vaporization are the active source processes on the first (quietest) day of our observations. Increased ion sputtering results whenever the magnetosphere opens in response to a southward interplanetary magnetic field (IMF) or unusually large solar wind dynamic pressure. The solar wind dynamic pressure at Mercury as inferred by heliospheric radial tomography increased by a factor 20 during this week, while the solar EUV flux measured by the Solar EUV Monitor (SEM) instrument on board the Solar and Heliospheric Observatory (SOHO) increased by 20%. While impact vaporization provides roughly 25% of the source, it is uniformly distributed and varies very little during the week. The variations seen in our data are not related to Caloris basin, which remained in the field of view during the entire week of observations. We conclude that increased ion sputtering resulting from ions entering the cusp regions is the probable mechanism leading to large rapid increases in the sodium content of the exosphere. While both the magnitude and distribution of the observed sodium can be reproduced by our model, in situ measurements of the solar wind density and velocity, the magnitude and direction of the interplanetary magnetic field, and Mercury's magnetic moments are required to confirm the results."

---
MARKER : "2001_solar_phys_202_81"
TYPE   : "in_journal"
AUTHOR : "Farnik, F., Karlicky, M., Svestka, Z."
AFFIL  : "CZECH-ONDREJOV, CZECH-ONDREJOV, {UCSD-CASS-SHPG, SRON-UTRECHT}"
TITLE  : "Locations of footpoints of transequatorial interconnecting loops"
SERIAL : "Solar Phys."
VOLUME : "202 (1)"
PAGE   : "81-98"
YEAR   : "2001-08"
DOI    : "10.1023/A:1011812000475"
TOPKEY : "solar activity"
ABS    : "We discuss footpoints of loops seen by Yohkoh in soft X-rays that connect active regions across the equator (transequatorial interconnecting loops - TILs). While most TILs are rooted in moderately strong fields at peripheries of active regions, there are also cases when these loops are anchored in very weak or very strong fields, ranging from &lt; 30 G to several hundred gauss. Some have their footpoints near sunspot penumbrae, creating 'X-ray fountains' in a combination with active region loops. But TILs are never rooted in sunspots. The most likely explanation is that magnetic field lines leave spots almost vertically so that TILs rooted in them extend high into the corona and density in them is below the limit of visibility in X-rays. The fact that in force-free modeling some TILs are rooted in sunspots is most probably due to the difference between field-line connections in 'vacuum' and in the highly conductive plasma on the Sun. Some TILs end before they reach active regions which sometimes may indicate the real situation, but mostly this 'gap' is probably due to a temperature decrease near the loop footpoints which makes them invisible in X-rays. In that case the fact that these cool lowest parts of TILs are never found in TRACE or SOHO EIT images indicates that plasma density in TILs must be very low. Still, the total absence of any counterparts of X-ray TILs in TRACE and EIT images is puzzling and, therefore, other possible interpretations of the 'gap' origin are also briefly mentioned."

---
MARKER : "2001_space_sci_rev_95_135"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
AFFIL  : "{UCSD-CASS-SHPG, SRON-UTRECHT}"
TITLE  : "Varieties of coronal mass ejections and their relation to flares"
SERIAL : "Space Sci. Rev."
VOLUME : "95 (1-2)"
PAGE   : "135-146"
YEAR   : "2001-01"
DOI    : "10.1023/A:1005225208925"
TOPKEY : "flares, coronal mass ejections"
ABS    : "Most coronal mass ejections (CMEs) start as coronal storms which are caused by an opening of channels of closed field lines along the zero line of the longitudinal magnetic field. This can happen along any zero line on the Sun where the configuration is destabilized. If the opening includes a zero line inside an active region, one observes a chromospheric flare. If this does not happen, no flare is associated with the CME in the chromosphere, but the process, as well as the response in the corona (a Long Decay Event in X-rays) remains the same. The only difference between flare-associated and non-flare-associated CMEs is the strength of the magnetic field in the region of the field line opening. This can explain essentially all differences which have been observed between these two kinds of CMEs. However, there are obviously also other sources of CMEs, different from coronal storms: sprays (giving rise to narrow, pointed ejections), erupting interconnecting loops (often destabilized by flares), and growing coronal holes. This paper tries to summarize and interpret observations which support this general picture, and demonstrates that both CMEs and flares must be properly discussed in any study of solar-terrestrial relations."

---
MARKER : "2001_space_sci_rev_97_35"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Hick, P.P., Jackson, B.V."
TITLE  : "Three-dimensional solar wind modeling using remote-sensing data"
SERIAL : "Space Sci. Rev."
VOLUME : "97"
PAGE   : "35-38"
EDITOR : "Marsden, R.G."
CTITLE : "34^th ESLAB Symposium: The 3-D heliosphere at solar maximum"
YEAR   : "2001"
TOPKEY : "IPS"
ABS    : "We have developed a computer-assisted tomography (CAT) technique that iteratively modifies a kinematic solar wind model to least-squares fit heliospheric remote sensing observations (interplanetary scintillation and Thomson-scattering observations). These remote sensing data cover a large range of solar elongations, and access high-latitude regions over the solar poles. The technique can be applied to a time-independent solar wind model, assuming strict co-rotation, or, when sufficient remote sensing observations are available, to a time-dependent model. For the time-dependent case the technique depends primarily on outward motion of structures in the solar wind to provide the perspective views required for a tomographic reconstruction. We show results of corotating tomographic reconstructions primarily using IPS velocity observations from the Solar-Terrestrial Environment Laboratory (STELab, Nagoya, Japan), and include comparisons with in situ velocity data out of the ecliptic (Ulysses) and in the ecliptic (ACE)"

---
MARKER : "2001_esa_sp_493_251"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Buffington, A., Hick, P.P."
TITLE  : "A heliospheric imager for Solar Orbiter"
EDITOR : "Battrick, B., Sawaya-Lacoste, H."
CTITLE : "Solar Encounter: the first Solar Orbiter workshop"
SERIAL : "ESA SP"
VOLUME : "493"
PAGE   : "251-256"
PUBLISH: "ESTEC, Noordwijk, The Netherlands"
YEAR   : "2001"
TOPKEY : "heliospheric imaging"
ABS    : "We have developed a prototype instrument for use on a near-Sun, three-axis stabilized, solar-oriented platform such as Solar Orbiter. The imager we envision analyzes remotely-sensed observations of coronal and heliospheric brightness in order to provide context for in situ plasma measurements. With this sensitive instrument, the analysis of these data will proceed much as it has from our recent use of Thomson-scattering observations from the Helios spacecraft, together with a recently developed time-dependent tomographic technique for analyzing these observations.

We show a full-scale optical prototype of our heliospheric imager for use on Solar Orbiter. We also show our most recent time-dependent tomographic result with Helios photometer data that depicts CMEs as well as corotating structures in the heliosphere and gives correlations of these data with in situ plasma density measurements at the spacecraft."

---
MARKER : "2000_encyclopedia_astron_astrophys_2290"
TYPE   : "in_book"
AUTHOR : "Svestka, Z."
TITLE  : "Solar flares: main phase"
EDITOR : "Murdin, P."
CTITLE : "Encyclopedia of Astronomy and Astrophysics"
PAGE   : "2290"
YEAR   : "2000-11"
URL    : "http://eaa.crcpress.com/default.asp?action=summary&articleId=2290"
DOI    : "10.1888/0333750888/2290"
TOPKEY : "flares"
ABS    : "After the impulsive phase of a flare is over (see SOLAR FLARES: IMPULSIVE PHASE), we talk about the main phase or gradual phase. Most FLARES (often called compact or confined flares) are short lived and they simply cool during the main phase, decaying within minutes or tens of minutes. However, there is also another kind of flares (eruptive flares) which continue to release energy during their ma..."

---
MARKER : "2000_applied_optics_39_2683"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Buffington, A."
TITLE  : "Improved design for stray-light reduction with a hemispherical imager"
SERIAL : "Applied Optics"
VOLUME : "39 (16)"
PAGE   : "2683-2686"
YEAR   : "2000-06"
DOI    : "10.1364/AO.39.002683"
TOPKEY : "heliospheric imaging"
ABS    : "We present a significant design improvement over previous visible-light stray-background-reducing baffles suitable for use on a stabilized deep-space platform. In earlier research we showed that when background-light sources are confined to a hemisphere or less, a conventional labyrinth baffle can be replaced by an array of concentric vanes, oriented away from the desired field of view. This configuration delivers substantial savings in size and weight. The present improvement replaces the concentric vanes by a smooth curved surface. This permits simplified fabrication and handling, provides even more weight reduction, and delivers improved performance for a given size. Laboratory measurements confirm stray-light performance with ~10<sup>-14</sup> rejection viewing as close as 3&deg; to a bright-light source."

---
MARKER : "2000_solar_phys_192"
TYPE   : "proceedings"
EDITOR : "Duvall jr., T.L., Harvey, J.W., Kosovichev, A.G., Svestka, Z."
TITLE  : "Proc. SOHO-9 Workshop on Helioseismic diagnostics of solar convection and activity"
PLACE  : "Stanford, CA, US, 12-15 July 1999"
SERIAL : "Solar Phys."
VOLUME : "192 (1-2)"
PAGE   : "(494 pages)"
YEAR   : "2000-03"
TOPKEY : "solar activity"
URL    : "http://www.springerlink.com/content/0038-0938/192/1-2/"

---
MARKER : "2000_yokhoh_soho_trace_jop_119"
TYPE   : "in_proceedings"
AUTHOR : "Farnik, F., Varady, M., Svestka, Z., Hudson, H., Fludra, A."
TITLE  : "Variability and physical properties of transequatorial interconnecting loops"
CTITLE : "Yohkoh, SOHO, TRACE JOP 119"
TOPKEY : "solar activity"
YEAR   : "2000-02"

---
MARKER : "2000_asr_25_1875"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Hick, P."
TITLE  : "Three dimensional tomography of heliospheric features using global Thomson scattering data"
EDITOR : "Watanabe, T., Schwenn, R."
CTITLE : "Coronal structure and dynamics near solar activity minimum"
SERIAL : "Adv. Space Res."
VOLUME : "25 (9)"
PAGE   : "1875-1878"
YEAR   : "2000"
DOI    : "10.1016/S0273-1177(99)00599-2"
TOPKEY : "Helios photometers"
ABS    : "Images of the heliosphere will become available from the Air Force/NASA Solar Mass Ejection Imager (SMEI), and from the all-sky cameras proposed for the NASA missions STEREO, Solar Probe and Solar Polar Sail. To optimize the information available from these instruments, their 2-dimensional images need to be interpreted in three dimensions. We have developed a Computer Assisted Tomography (CAT) program that modifies a three-dimensional heliospheric model to fit Thomson scattering solar minimum observations from the Helios spacecraft photometers. The tomography program iterates to a least-squares solution fit of observed brightness data using spacecraft and solar wind motion to provide perspective views of each point in space accessible to the observations. We plot the optimized models as Carrington maps in density for the Helios data sets. The results to date are commensurate with resolutions available from the original data. At solar minimum, longitudinally segmented dense structures emanate from near the solar equator. We explore the location of these dense structures with respect to the heliospheric current sheet and regions of activity on the solar surface."

---
MARKER : "1999_current_science_77_1503"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Solar activity: an overview"
SERIAL : "Current Science"
VOLUME : "77 (11)"
PAGE   : "1503-1510"
YEAR   : "1999-12"

---
MARKER : "1999_esa_sp_446_61"
TYPE   : "in_proceedings"
AUTHOR : "Svestka, Z."
TITLE  : "Solar activity on all scales"
EDITOR : "Vial, J.-C., Kaldeich-Schurmann, B."
CTITLE : "Proc. 8^th SOHO Workshop on Plasma dynamics and diagnostics in the solar transition region and corona"
PLACE  : "Paris, France, 22-26 June 1999"
SERIAL : "ESA SP"
VOLUME : "446"
PAGE   : "61"
YEAR   : "1999-10"
URL    : "http://adsabs.harvard.edu/abs/1999ESASP.446...61S"

---
MARKER : "1999_esa_sp_446_103"
TYPE   : "in_proceedings"
AUTHOR : "Clette, F., Poletto, G., Ŝvestka, Z."
TITLE  : "Working group 6: activity on all scales"
EDITOR : "Vial, J.-C., Kaldeich-Schürmann, B."
CTITLE : "Proc. 8^th SOHO Workshop on Plasma dynamics and diagnostics in the solar transition region and corona"
PLACE  : "Paris, France, 22-26 June 1999"
SERIAL : "ESA SP"
VOLUME : "446"
PAGE   : "103"
YEAR   : "1999-10"
URL    : "http://adsabs.harvard.edu/abs/1999ESASP.446..103C"

---
MARKER : "1999_esa_sp_446_305"
TYPE   : "in_proceedings"
AUTHOR : "Farnik, F., Svestka, Z., Karlický, M., Hudson, H.S."
TITLE  : "Transequatorial interconnecting loops and increase of their length in the new cycle"
EDITOR : "Vial, J.-C., Kaldeich-Schurmann, B."
CTITLE : "Proc. 8^th SOHO Workshop on Plasma dynamics and diagnostics in the solar transition region and corona"
PLACE  : "Paris, France, 22-26 June 1999"
SERIAL : "ESA SP"
VOLUME : "446"
PAGE   : "305"
YEAR   : "1999-10"
URL    : "http://adsabs.harvard.edu/abs/1999ESASP.446..305F"

---
MARKER : "1999_solar_phys_188_217"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Book review"
SERIAL : "Solar Phys."
VOLUME : "188 (1)"
PAGE   : "217"
YEAR   : "1999-08"
DOI    : "10.1023/A:1005113510227"
REMARK : "book review"

---
MARKER : "1999_solar_phys_187_33"
TYPE   : "in_journal"
AUTHOR : "Farnik, F., Karlicky, M., Svestka, Z."
TITLE  : "Long transequatorial interconnecting loops of the new solar cycle"
SERIAL : "Solar Phys."
VOLUME : "187 (1)"
PAGE   : "33-44"
YEAR   : "1999-06"
DOI    : "10.1023/A:1005123319045"

---
MARKER : "1999_aip_sw9_471_565"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Yokobe, A., Ohmi, T., Hakamada, K., Kojima, M., Tokumaru, M., Jackson, B.V., Hick, P.P., Zidowitz, S."
TITLE  : "Comparison of solar wind speed with coronagraph data analyzed by tomography"
EDITOR : "Habbal, S.R., Esser, R., Hollweg, J.V., Isenberg, P.A."
CTITLE : "Solar Wind Nine"
SERIAL : "AIP Conf. Proc."
VOLUME : "471"
PAGE   : "565-567"
YEAR   : "1999"
DOI    : "10.1063/1.58811"
TOPKEY : "IPS"
ABS    : "We have analyzed the relation between solar wind speeds observed by interplanetary scintillation (IPS) and coronal densities derived from coronagraph observations during the 'Whole Sun Month' period in 1996. Since both IPS and coronagraph observations are biased by the effect of line-of-sight integration, tomography techniques are applied to both data sets. For this analysis we made a synoptic map of the solar wind speed at the source surface (2.5 R_sun) from the IPS tomography. Each speed region on the source surface was traced to the height of the coronagraph observations along the magnetic field lines calculated from the source surface potential field model. This analysis has obtained clear anti-correlation between the solar wind speed in interplanetary space and electron density at lower coronal regions. We have also obtained the radial profiles of coronal densities for both slow and fast wind flows in the range of 1.3&minus;2.0 R_Sun. We expect that these provide experimental constraints on solar wind acceleration models."

---
MARKER : "1999_aip_sw9_471_231"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Hick, P., Svestka, Z, Jackson, B.V., Farnik, F., Hudson, H."
TITLE  : "Quiet solar wind signatures above active regions observed in X-rays"
EDITOR : "Habbal, S.R., Esser, R., Hollweg, J.V., Isenberg, P.A."
CTITLE : "Solar Wind Nine"
SERIAL : "AIP Conf. Proc."
VOLUME : "471"
PAGE   : "231-233"
YEAR   : "1999"
DOI    : "10.1063/1.58752"
TOPKEY : "solar wind, corona"
ABS    : "X-ray images from the Yohkoh satellite, obtained following occurrences of limb flares sometimes show coronal fan-like structures extending above a growing post-flare loop system. We show one such event observed in AR 7270 on the east limb of the Sun on 28/29 August 1992. We suggest that these rays are 'ministreamers', formed as a result of the restructuring of the corona following the occurrence of a flare-associated CME. Synoptic maps of the solar wind density, constructed from a tomographic analysis of interplanetary scintillation (IPS) measurements, show enhanced scintillation matching the position of AR 7270 if we assume a radial outflow at a reasonable slow solar wind speed of 400 km s^-1.  From this agreement we argue that outflow of mass occurs from the active region into interplanetary space."

---
MARKER : "1999_faces_of_the_sun_chapter_12"
TYPE   : "in_book"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Svestka, Z., Poletto, G, Fontenla, J., Hick, P., Kopp, R.A., Sylwester, B., Sylwester, J."
TITLE  : "Flares: The gradual phase"
EDITOR : "Strong, K., Saba, J., Haisch, B., Schmelz, J."
CTITLE : "The many faces of the Sun"
CHAPTER: "12"
PUBLISH: "Springer Verlag, New York"
PAGE   : "409-439"
YEAR   : "1999-00"
TOPKEY : "corona, flares"
ABS    : "We discuss the processes of heating and cooling in the gradual phase of flares, and demonstrate the method of deriving emission measure &minus; temperature diagrams. The new phenomena of flaring and giant post-flare arches discovered using data from the Solar Maximum Mission (SMM) Hard X-ray Imaging Spectrometer (HXIS) are discussed, and we summarize our present knowledge about the gradual phase of eruptive flares."

---
MARKER : "1998_spie_3442_87"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Hick, P.P., Jackson, B.V."
TITLE  : "Three dimensional tomography of heliospheric features using Thomson scattering data"
EDITOR : "Korendyke, C.M."
CTITLE : "Missions to the Sun II"
SERIAL : "Proc. SPIE"
VOLUME : "3442"
PAGE   : "87-93"
YEAR   : "1998-11"
DOI    : "10.1117/12.330246"
TOPKEY : "Helios photometers"
ABS    : "All-sky cameras for viewing the heliosphere in white light are included in the design of several future spacecraft missions. The first of these to be put in Earth-orbit will be the Solar Mass Ejection Imager (SMEI), a joint project of the US Air Force, NASA and the University of Birmingham, UK. Other missions, including an all-sky imager in their current design, are STEREO, Solar Probe and Solar Polar Sail. The white-light signal includes Thomson-scattered light from heliospheric electrons, which can be used to study the structure and evolution of large-scale heliospheric features. These studies are the principal reason for putting all-sky cameras in Earth-orbit or deep space. We discuss a tomographic technique, which uses the two-dimensional information in the all-sky images provided by these cameras to reconstruct the heliospheric density structure in three dimensions. We present preliminary results of this tomographic technique applied to Thomson scattering data from the photometers onboard the two HELIOS spacecraft."

---
MARKER : "1998_spie_3442_77"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Buffington, A., Hick, P., Jackson, B.V., Korendyke, C.M."
TITLE  : "Corrals, hubcaps, and crystal balls: some new designs for very wide-angle visible-light heliospheric imagers"
EDITOR : "Korendyke, C.M."
CTITLE : "Missions to the Sun II"
SERIAL : "Proc. SPIE"
VOLUME : "3442"
PAGE   : "77-86"
YEAR   : "1998-11"
DOI    : "10.1117/12.330266"
TOPKEY : "heliospheric imaging"
ABS    : "Emerging techniques allow instruments to view very large sky areas, a hemisphere or more, in visible light. In space, such wide-angle coverage enables observation of heliospheric features form close to the Sun to well beyond Earth. Observations from deep-space missions such as Solar Probe, Stereo, and Solar Polar Sail, coupled with observations near Earth, permit 3D reconstruction of solar mass ejections and co-rotating structures, discovery and study of new comets and asteroids, and detailed measurements of brightness variations in the zodiacal cloud. Typical heliospheric features have 1 percent or less of ambient brightness, so visible-light cameras must deliver < 0.1 percent photometry and be well protected from stray background light. When more than a hemisphere of viewing area is free of bright background-light sources, we have shown that corral-like structures with several vane-like walls reduces background light illuminating to wide-angle optical system by up to ten orders of magnitude. The optical system itself typically provides another five orders of surface-brightness reduction. With CCDs as the light-detection device, images of point-like sources must cover typically 100 pixels to average down sub-pixel response gradients and provide the above 0.1 percent photometry. With present-day CCDs this requires images of order 1 degree in angular size. Tolerating such large images in turn enables wide-angle sky coverage using simple reflecting and refracting optical systems such as convex spherical reflectors, toroids and thick lenses. We show that combining these with light- reducing corrals yields practical, light-weight instruments suitable for inclusion on deep-space probes."

---
MARKER : "1998_apj_505_984"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Leinert, C., Jackson, B.V."
TITLE  : "Global solar wind changes over Solar Cycle 21: A combination of Helios photometer, In situ, and interplanetary scintillation data"
SERIAL : "Astrophys. J."
VOLUME : "505 (2)"
PAGE   : "984-992"
YEAR   : "1998-10"
DOI    : "10.1086/306180"
TOPKEY : "Helios photometers, IPS"
ABS    : "We combine Helios spacecraft photometer brightnesses, in situ plasma densities, and interplanetary scintillation (IPS) velocity data to obtain a global description of solar wind changes. We find an increase of solar mass flux at solar maximum from the photometer brightnesses larger than would be expected from the usual assumption of invariant momentum flux over solar cycle 21 (1975-1986). A portion of this excess mass is related to solar mass ejections, which have an occurrence rate that follows the solar activity cycle."

---
MARKER : "1998_solar_phys_182_179"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Svestka, Z., Farnik, F., Hudson, H.S., Hick, P."
TITLE  : "Large scale active coronal phenomena in Yohkoh SXT images, IV. Solar wind streams from flaring active regions"
SERIAL : "Solar Phys."
VOLUME : "182 (1)"
PAGE   : "179-193"
YEAR   : "1998-09"
DOI    : "10.1023/A:1005033717284"
TOPKEY : "corona"
ABS    : "We demonstrate limb events on the Sun in which growing flare loop systems are embedded in hot coronal structures looking in soft X-rays like fans of coronal rays. These structures are formed during the flare and extend high into the corona. We analyze one of these events, on 28-29 August 1992, which occurred in AR 7270 on the eastern limb, and interpret these fans of rays either as temporary multiple ministreamers or plume-like structures formed as a result of restructuring due to a CME. We suggest that this configuration reflects mass flow from the active region into interplanetary space. This suggestion is supported by synoptic maps of solar wind sources constructed from scintillation measurements which show a source of enhanced solar wind density at the position of AR 7270, which disappears when 5 days following the event are removed from the synoptic map data. We also check synoptic maps for two other active regions in which existence of these fan-like structures was indicated when the active regions crossed both the east and west limbs of the Sun, and both these regions appear to be sources of a density enhancement in the solar wind."

---
MARKER : "1998_applied_optics_37_4284"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Buffington, A."
TITLE  : "Very-wide-angle optical systems suitable for spaceborne photometric measurements"
SERIAL : "Applied Optics"
VOLUME : "37 (19)"
PAGE   : "4284-4293"
YEAR   : "1998-07"
DOI    : "10.1364/AO.37.004284"
TOPKEY : "heliospheric imaging"
ABS    : "Spaceborne visible-light images for observing the large angular extent of the solar corona require 0.1% differential broadband photometry over ~1&deg; sky bins. When we are using a CCD camera, this specification requires spreading unresolved images over many pixels. Large images ease correction for aberration or field curvature. Permitting large images allows simple and lightweight very-wide-angle designs employing spherical and toroidal mirrors and thick lenses that can view almost the entire sky. We present formulas and graphic results relating sky angle to focal-plane position and determining the tangential and sagittal focal surfaces governing image size at the CCD. Laboratory measurements with two prototype configurations confirm the calculations."

---
MARKER : "1998_jgr_103_12049"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Hick, P.L., Kojima, M., Yokobe, A."
TITLE  : "Heliospheric tomography using interplanetary scintillation observations, 1. Combined Nagoya and Cambridge observations"
SERIAL : "J. Geophys. Res."
VOLUME : "103 (A6)"
PAGE   : "12049-12067"
YEAR   : "1998-06"
DOI    : "10.1029/97JA02528"
TOPKEY : "IPS"
ABS    : "We have produced a computer assisted tomography program that optimizes a three-dimensional model to fit observational data. We have used this program with interplanetary scintillation data from Nagoya, Japan, and Cambridge, England. The program iterates to a least squares solution fit of observed data using solar rotation and solar wind motion to provide perspective views of each point in space accessible to the observations. We plot the optimized model as Carrington maps in velocity V and density for the two data sets with resolutions of 10&deg; in heliographic longitude and latitude. We map the model to 1 AU and compare this to in situ observations from the IMP spacecraft. From this comparison we find &delta;N_e&prop;N_e^0.3. We plot Carrington maps extrapolated to the solar surface to compare with Yohkoh Soft X ray Telescope (SXT), Sacramento Peak green line, and Mark III K-coronameter observations. High velocities modeled at the solar surface for individual rotations trace coronal holes (including polar ones) observed in SXT data. Regions of high density modeled from the Cambridge scintillation level data generally show a high correlation with regions of high solar activity observed as bright in Yohkoh SXT and green line observations. There is also a general correspondence of the regions of high density and the areas which are bright in K-coronameter observations."

---
MARKER : "1998_jgr_103_1991"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Asai, K., Kojima, M., Tokumaru, M., Yokobe, A., Jackson, B.V., Hick, P.L."
TITLE  : "Heliospheric tomography using interplanetary scintillation observations, 3. Correlation between speed and electron density fluctuations in the solar wind"
SERIAL : "J. Geophys. Res."
VOLUME : "103 (A2)"
PAGE   : "1991-2001"
YEAR   : "1998-02"
DOI    : "10.1029/97JA02750"
TOPKEY : "IPS"
ABS    : "We have examined the relationship between solar wind speed and electron density fluctuations on scale sizes around 100 km in the heliocentric distance range of 0.3 to 0.8 AU using interplanetary scintillation (IPS) data obtained at the Solar-Terrestrial Environment Laboratory. The solar wind properties derived from the IPS data are biased by line of sight integration through a three-dimensional structured solar wind. Therefore we have applied a computer-assisted tomography (CAT) method to deconvolve the line of sight integration and reconstruct the solar wind structure. The analysis was made for the solar wind speed V and electron density fluctuations &delta;N_e in the solar activity minimum phase when high-speed regions are separated from an equatorial low-speed region by a sharp velocity gradient. From results of the CAT analysis we derived the best fit power law relation of &delta;N_e&prop;V^&minus;&gamma; with &gamma;=0.5&plusmn;0.15, indicating that fractional density fluctuations &delta;N_e/N_e in the high-speed wind are larger than those in the low-speed wind. Combining this relation with results of previous workers [Coles et al., 1995; Manoharan, 1993; Celnikier et al., 1987; Jackson et al., 1998], we suggest that the fractional density fluctuation level of the high-speed wind evolves with heliocentric distance."

---
MARKER : "1998_jgr_103_1981"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Kojima, M., Tokumaru, M., Watanabe, H., Yokobe, A., Jackson, B.V., Hick, P.L."
TITLE  : "Heliospheric tomography using interplanetary scintillation observations, 2. Latitude and heliocentric distance dependence of solar wind structure at 0.1-1 AU"
SERIAL : "J. Geophys. Res."
VOLUME : "103 (A2)"
PAGE   : "1981-1989"
YEAR   : "1998-02"
DOI    : "10.1029/97JA02162"
TOPKEY : "IPS"
ABS    : "Interplanetary scintillation is a useful means to measure the solar wind in regions inaccessible to in situ observation, However, interplanetary scintillation measurements involve a line-of-sight integration, which relates contributions from all locations along the line of sight to the actual observation. We have developed a computer assisted tomography (CAT) program to reduce the adverse effects of the line-of-sight integration. The program uses solar rotation and solar wind motion to provide three-dimensional perspective views of each point in space accessible to the interplanetary scintillation observations and optimizes a three-dimensional solar wind speed distribution to fit the observations. We analyzed IPS speeds observed at the Solar-Terrestrial Environment Laboratory and confirmed that (1) the solar wind during the solar minimum phase has a dominant polar high-speed solar wind region with speeds of about 800 km s^&minus;1 and within 30 degrees of the solar equator speeds decrease to 400 km s^&minus;1 as observed by Ulysses, and (2) high-speed winds get their final speed of 750&minus;900 km s^&minus;1 within 0.1 AU, and consequently, that acceleration of the solar wind is small above 0.1 AU."

---
MARKER : "1998_aasup_127_001"
TYPE   : "in_journal"
AUTHOR : "Leinert, C., Bowyer, S., Haikala, L.K., Hanner, M.S., Hauser, M.G., Levasseur-Regourd, A.-Ch., Mann, I., Mattila, K., Reach, W.T., Schlosser, W., Staude, H.J., Toller, G.N., Weiland, J.L., Weinberg, J.L., Witt, A.N."
TITLE  : "The 1997 reference of diffuse night sky brightness"
SERIAL : "Astron. Astrophys. Sup."
VOLUME : "127 (1)"
PAGE   : "1-99"
YEAR   : "1998-01"
DOI    : "10.1051/aas:1998105"
TOPKEY : "zodiacal light"
ABS    : "In the following we present material in tabular and graphical form, with the aim to allow the non-specialist to obtain a realistic estimate of the diffuse night sky brightness over a wide range of wavelengths from the far UV longward of Ly &alpha; to the far-infrared. At the same time the data are to provide a reference for cases in which background brightness has to be discussed, including the planning for space observations and the issue of protection of observatory sites. We try to give a critical presentation of the status at the beginning of 1997."

---
MARKER : "1998_soltip_3_207"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Kojima, M., Asai, K., Jackson, B.V., Hick, P.L., Tokumaru, M., Watanabe, H., Yokobe, A."
TITLE  : "Solar wind structure at 0.1-1 AU reconstructed from IPS observations using tomography"
EDITOR : "Feng, X.S., Wei, F.S., Dreyer, M."
CTITLE : "3^rd SOLTIP Symp. On Solar Transient Phenomena (Bejing, China, 14-18 October, 1996)"
PAGE   : "207-212"
PUBLISH: "International Academic Publ."
YEAR   : "1998"
TOPKEY : "IPS"

---
MARKER : "1998_assl_229_365"
TYPE   : "in_proceedings"
AUTHOR : "Svestka, Z., Farnik, F."
TITLE  : "Post-flare structures rising with decreasing or constant speed"
CTITLE : "Proc. on Observational plasma astrophysics: five years of Yohkoh and beyond"
PLACE  : "Tokyo, Japan, 6-8 November 1996"
SERIAL : "Astrophysics and Space Science Library"
VOLUME : "229"
PAGE   : "365-369"
YEAR   : "1998-00"

---
MARKER : "1998_40_years_of_cospar_75"
TYPE   : "in_book"
AUTHOR : "Svestka, Z."
TITLE  : "A window to the west"
EDITOR : "Haerendel, G., Grzedzielski, S., Cavallo, G., Battrick, B."
CTITLE : "40 years of COSPAR"
PAGE   : "75"
YEAR   : "1998-00"
PUBLISH: "ESA"

---
MARKER : "1997_solar_phys_176_355"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Svestka, Z., Farnik, F., Hick, P., Hudson, H.S., Uchida, Y."
TITLE  : "Large scale active coronal phenomena in Yohkoh SXT images, III. Enhanced post-flare streamer"
SERIAL : "Solar Phys."
VOLUME : "176 (2)"
PAGE   : "355-371"
YEAR   : "1997-12"
DOI    : "10.1023/A:1004938329182"
TOPKEY : "corona"
ABS    : "We demonstrate several events where an eruptive flare close to the limb gave rise to a transient coronal streamer visible in X-rays in Yohkoh SXT images, and analyze one of these events, on 28&minus;29 October 1992, in detail. A coronal helmet streamer began to appear 2 hours after the flare, high above rising post-flare loops; the streamer became progressively narrower, reaching its minimum width 7&minus;12 hours after the flare, and widened again thereafter, until it eventually disappeared. Several other events behaved in a similar way. We suggest that the minimum width indicates the time when the streamer became fully developed. All the time the temperature in the helmet streamer structure was decreasing, which can explain the subsequent fictitious widening of the X-ray streamer. It is suggested that we may see here two systems of reconnection on widely different altitudes, one giving rise to the post-flare loops while the other creates (or re-forms) the coronal helmet streamer. A similar interpretation was suggested in 1990 by Kopp and Poletto for post-flare giant arches observed on board the SMM; indeed, there are some similarities between these post-flare helmet streamers and giant arches and, with the low spatial resolution of SMM instruments, it is possible that some helmet streamers could have been considered to be a kind of a giant arch."

---
MARKER : "1997_solar_phys_175"
TYPE   : "proceedings"
EDITOR : "Fleck, B., Svestka, Z."
TITLE  : "Topical issue 'The first results from SOHO'"
SERIAL : "Solar Phys."
VOLUME : "175 (2)"
PAGE   : "(799)"
YEAR   : "1997-10"
URL    : "http://www.springerlink.com/content/0038-0938/175/2/"

---
MARKER : "1997_solar_phys_170_321"
TYPE   : "in_journal"
AUTHOR : "Neidig, D.F., Svestka, Z., Cliver, E.W., Airapetian, V., Henry, T.W."
TITLE  : "Observations of faint, outlying loop systems in large flares"
SERIAL : "Solar Phys."
VOLUME : "170 (2)"
PAGE   : "321-339"
YEAR   : "1997-02"
DOI    : "10.1023/A:1004923212539"

---
MARKER : "1997_esa_sp_415_139"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Svestka, Z., Farnik, F., Hudson, H.S., Hick, P."
TITLE  : "Post-flare loops embedded in a hot coronal fan-like structure"
EDITOR : "Wilson, A."
CTITLE : "31^st ESLAB Symposium: Correlated phenomena at the Sun, in the heliosphere and in geospace"
SERIAL : "ESA SP"
VOLUME : "415"
PAGE   : "139-144"
PUBLISH: "ESTEC, Noordwijk, Netherlands"
YEAR   : "1997"
TOPKEY : "post-flare arch, flares"
ABS    : "We demonstrate limb events on the Sun in which rising post-flare loops were embedded in hot structures looking in soft X-rays like fans of rays, formed during the flare and extending high into the corona. We analyze one of these structures and suggest that these fans of rays represent temporary ministreamers, along which mass is flowing into interplanetary space. This suggestion is supported by maps of solar wind density constructed from scintillation measurements."

---
MARKER : "1997_phys_chem_earth_22_425"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Hick, P., Kojima, M., Yokobe, A."
TITLE  : "Heliospheric tomography using interplanetary scintillation observations"
SERIAL : "Physics and Chemistry of the Earth"
VOLUME : "22 (5)"
PAGE   : "425-434"
YEAR   : "1997"
DOI    : "10.1016/S0079-1946(97)00170-5"
TOPKEY : "IPS"
ABS    : "We have produced a Computer Assisted Tomography (CAT) program that optimizes a three dimensional solar wind velocity, V, and density fluctuation, Ne, model to fit observed interplanetary scintillation (IPS) data from Nagoya, Japan and Cambridge, England.  The multiple perspective views of the solar wind needed for the reconstruction solution are provided by solar rotation and outward solar wind motion. The CAT program iterates to a least squares fit solution to the observed IPS values. We map the model to one AU and compare this to in situ observations from the IMP spacecraft. From this comparison we find &delta;N_e&prop;N_e^0.3. We plot the optimized model as Carrington maps in velocity and &delta;N_e, and compare these with Yohkoh Carrington synoptic maps. We find that the model velocity projected to the solar surface for individual rotations shows regions of high velocity that map directly to coronal hole areas observed in Yohkoh Soft X-ray Telescope (SXT) observations. Regions of slow velocity generally map to bright regions in SXT data. Regions of high Ne show a high correlation with regions of high solar activity observed as bright in Yohkoh SXT observations."

---
MARKER : "1997_phys_chem_earth_22_441"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Buffington, A., Hick, P., Kahler, S.W., Keil, S.L., Simnett, G., Webb, D.F."
TITLE  : "The Solar Mass Ejection Imager"
SERIAL : "Physics and Chemistry of the Earth"
VOLUME : "22 (5)"
PAGE   : "441-444"
YEAR   : "1997"
DOI    : "10.1016/S0079-1946(97)00172-9"
TOPKEY : "Coriolis-SMEI"
ABS    : "We are designing a Solar Mass Ejection Imager (SMEI) capable of observing Thomson-scattered signals from heliospheric density features from a spacecraft situated near 1 AU. The imager is designed to trace these features, which include coronal mass ejections, corotating structures and shock waves, to elongations greater than 90&deg; from the Sun. The instrument may be regarded as a progeny of the heliospheric imaging capability shown possible by the zodiacal light photometers of the HELIOS spacecraft. The instrument we are designing would make more effective use of in situ solar wind data from spacecraft in the vicinity of the imager by extending their observations to the surrounding environment. An imager at Earth could allow up to three days warning of the arrival of a mass ejection from the Sun. In combination with similar instruments in deep space SMEI can be used for stereoscopic imaging of heliospheric features."

---
MARKER : "1997_asr_20_23"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Hick, P.L., Kojima, M., Yokobe, A."
TITLE  : "Heliospheric tomography using interplanetary scintillation observations"
EDITOR : "Antonucci, E., Page, D.E."
CTITLE : "The Sun and its role in the heliosphere"
SERIAL : "Adv. Space Res."
VOLUME : "20 (1)"
PAGE   : "23-26"
YEAR   : "1997"
DOI    : "10.1016/S0273-1177(97)00474-2"
TOPKEY : "IPS"
ABS    : "We have produced a Computer Assisted Tomography (CAT) program that optimizes a three-dimensional model to fit observational data. We have used this program with interplanetary scintillation data from Nagoya, Japan and Cambridge, England. The program iterates to a least-squares solution fit of observed data using solar rotation and solar wind motion to provide perspective views of each point in space accessible to the observations. We plot the optimized model as Carrington maps in velocity, V, and density, N_e, for the two data sets with resolutions of ten degrees in heliographic longitude and latitude. High velocities modeled at the solar surface for individual rotations trace the outlines of coronal holes (including polar ones) observed in Yohkoh Soft X-ray Telescope (SXT) observations. Regions of slow velocity generally map to bright regions in SXT data. Regions of high density modeled from the Cambridge scintillation level data generally show a high correlation with regions of high solar activity observed as bright in Yohkoh SXT observations."

---
MARKER : "1997_aspcs_111_388"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Svestka, Z., Farnik, F., Hudson, H.S., Uchida, Y., Hick, P."
TITLE  : "Large-scale active coronal phenomena in YOHKOH SXT images"
EDITOR : "Bentley, R.D., Mariska, J.T."
CTITLE : "Magnetic reconnection in the solar atmosphere"
SERIAL : "ASP Conf. Series"
VOLUME : "111"
PAGE   : "388-392"
YEAR   : "1997"
TOPKEY : "corona"
ABS    : "We have checked in Yohkoh SXT images the appearance of giant post-flare arches which were discovered in hard X-ray images from the HXIS and FCS instruments onboard the SMM. We have verified the existence of both the rising and stationary arches. In addition to these two kinds of giant post-flare arches, known before from SMM observations, Yohkoh also reveals other large post-flare coronal structures which might have been considered to be giant arches by the low-resolution SMM instruments. These include coronal helmet streamers above rising flare loops or fans of hot structures in which the rising loops are embedded."

---
MARKER : "1997_aip_385_97"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Kojima, M., Asai, K., Hick, P.L., Jackson, B.V., Tokumaru, M., Watanabe, H., Yokobe, A."
TITLE  : "Solar wind structure at 0.1-1 AU reconstructed from IPS observations using tomography"
EDITOR : "Habbal, S.R."
CTITLE : "Robotic exploration close to the Sun: Scientific basis"
SERIAL : "AIP Conf. Proc."
VOLUME : "385"
PAGE   : "97-104"
YEAR   : "1997-01"
DOI    : "10.1063/1.51771"
TOPKEY : "IPS"
ABS    : "Although interplanetary scintillation (IPS) is a useful means to measure the solar wind in regions where spacecraft cannot access, the IPS measurement requires a line of sight integration to relate what is observed to a location in space. We have produced a Computer Assisted Tomography (CAT) program that optimizes a three-dimensional solar wind speed distribution to fit observed interplanetary scintillation data from STE Lab. Nagoya University. The program uses solar rotation and solar wind motion to provide 3-dimensional perspective views of each point in space accessible to the IPS observations and iterates to a least-square solution fit of the observations. We plot the optimized result as a Carrington map of solar wind speed at a height of 2.5 Rs and have confirmed (1) the solar wind near a solar minimum phase has a bimodal structure near the sun, that is, a low-speed region and a high-speed region are separated by a sharp speed gradient, (2) high-speed winds get their final speed of 750&minus;800 km/s within 0.1 AU, and subsequently the evolution of solar wind structure is small at 0.1&minus;1AU."

---
MARKER : "1997_stp5_188"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Webb, D.F., Jackson, B.V., Hick, P."
TITLE  : "Effects of CMEs on the heliosphere and geomagnetic storms using Helios data"
EDITOR : "Heckman, G., Maruboshi, K., Shea, M.A., Smart, D.F., Thompson, R."
CTITLE : "Solar-Terrestrial Predictions V"
PAGE   : "188"
YEAR   : "1997"
TOPKEY : "Helios photometers"

---
MARKER : "1996_solar_phys_169_403"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Speeds of rising post-flare structures"
SERIAL : "Solar Phys."
VOLUME : "169 (2)"
PAGE   : "403-413"
YEAR   : "1996-12"
DOI    : "10.1007/BF00190616"

---
MARKER : "1996_applied_optics_35_6669"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Buffington, A., Jackson, B.V., Korendyke, C.M."
TITLE  : "Wide-angle stray-light reduction for a spaceborne optical hemispherical imager"
SERIAL : "Applied Optics"
VOLUME : "35 (34)"
PAGE   : "6669-6673"
YEAR   : "1996-12"
DOI    : "10.1364/AO.35.006669"
TOPKEY : "heliospheric imaging"
ABS    : "We describe a simple visible-light stray-background-reducing baffle, suitable for use on a stabilized interplanetary platform. The design is a corrallike enclosure with five concentric walls. The baffle reduces direct sunlight and reflections from illuminated portions of the spacecraft by a factor of 10-12, provided that all these lie beyond at least a hemisphere centered on the viewing aperture. With this condition these bright sources do not directly illuminate within the outermost wall of the corral, and diffraction over the wall tops is the dominant mechanism by which light reaches the corral interior. We present design calculations for such a corral, as well as a laboratory measurement confirming the basic design assumption."

---
MARKER : "1996_solar_phys_169_225"
TYPE   : "in_journal"
AUTHOR : "Howard, R.F., van den Oord, G.H.J., Svestka, Z."
TITLE  : "Book reviews"
SERIAL : "Solar Phys."
VOLUME : "169 (1)"
PAGE   : "225-227"
YEAR   : "1996-11"
DOI    : "10.1007/BF00153843"
REMARK : "book review"

---
MARKER : "1996_solar_phys_168_331"
TYPE   : "in_journal"
AUTHOR : "Farnik, F., Svestka, Z., Hudson, H.S., Uchida, Y."
TITLE  : "Large-scale active coronal phenomena in Yohkoh SXT images, II: Stationary post-flare giant arches"
SERIAL : "Solar Phys."
VOLUME : "168 (2)"
PAGE   : "331-343"
YEAR   : "1996-10"
DOI    : "10.1007/BF00148059 "

---
MARKER : "1996_iau_153_609"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Svestka, Z., Farnik, F., Hudson, H.S., Uchida, Y., Hick, P., Lemen, J.R."
TITLE  : "Large-scale active coronal phenomena in YOHKOH SXT images"
EDITOR : "Uchida, Y., Kosugi, T., Hudson, H.S."
CTITLE : "Proc. 153^rd IAU Coll. on Magnetodynamic phenomena in the solar atmosphere: Prototypes of stellar magnetic activity"
PAGE   : "609-610"
PUBLISH: "Kluwer Academic Publ., Dordrecht, Netherlands"
YEAR   : "1996-03"
TOPKEY : "corona"
ABS    : "We have found several occurrences of slowly expanding giant arches in Yohkoh images. These are similar to the giant post-flare arches previously discovered by SMM instruments in the 80s. However, we see them now with 3&times;5 better spatial resolution and can recognize well their loop-like structure. As a rule, these arches follow eruptive flares with gradual soft X-ray bursts and rise with speeds in the range of 1.1&minus;2.4 km s^&minus;1 which keep constant for &gt;5 to 24 hours, reaching altitudes up to 250,000 km above the solar limb. These arches differ from post-flare loop systems by their (much higher) altitudes, (much longer) lifetimes, and (constant) speed of growth. One event appears to be a rise of a transequatorial interconnecting loop.

In the event of 21&minus;22 February 1992 one can see both the loop system, rising with a gradually decreasing speed to an altitude of 120,000 km, and the arch, emerging from behind the loops and continuing to rise with a constant speed for many more hours up to 240,000 km above the solar limb. In the event of 2&minus;3 November 1991 three subsequent rising large-scale coronal systems can be recognized: first a fast one with speed increasing with altitude and ceasing to be visible at about 300,000 km. This most probably shows the X-ray signature of a coronal mass ejection (CME). A second one, with gradually decreasing speed, might represent very high rising flare loops. A third one continues to rise slowly with a constant speed up to 230,000 km (and up to 285,000 km after the speed begins to decay), and this is the giant arch. This event, including an arch revival on November 4&minus;5, is very similar to rising giant arches observed by the SMM on 6&minus;7 November 1980. Other events of this kind were observed on 27&minus;28 April 1992, 15 March 1993, and 4&times;6 November 1993, all seen above the solar limb, where it is much easier to identify them.

The temperature in the brightest part of the arch of 2&times;3 November 1991 was increasing with its altitude, from 2 to 4&times;10^6 K, which seems to be an effect of slower cooling at lower densities. Under the assumption of a line-of-sight thickness of 50,000 km, the emission measure indicates arch densities from 1.1&times;10^10 cm^&minus;3 at an altitude of 150,000 km to 1.0&times;10^9 cm^&minus;3 at 245,000 km 11.5 hours later. It appears that the arch is composed of plasma of widely different temperatures, and that hot plasma rises faster than the cool component. Thus the whole arch expands upward and its density gradient increases with time which explains why Yohkoh images show only the lowest and coolest parts of the expanding structure. The whole arch may represent an energy in excess of 10^31 erg, and more if conduction contributes to the arch cooling.

We suggest that the rise of the arch is initiated by a CME which removes the magnetic field and plasma in the upper corona and the coronal structures remaining below this cavity begin to expand into the 'magnetic vacuum' left behind the CME. However, we are unable to explain why the speed of rise stays constant for so many hours.

The complete paper will appear in Solar Phys. 160, issue 2 (November 1995)."

---
MARKER : "1996_spie_2804_78"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Keil, S.L., Altrock, R.C., Kahler, S.W., Jackson, B.V., Buffington, A., Hick, P.L., Simnett, G., Eyles, C., Webb, D.F., Anderson, P."
TITLE  : "The Solar Mass Ejection Imager (SMEI)"
EDITOR : "Rust, D."
CTITLE : "Missions to the Sun"
SERIAL : "Proc. SPIE"
VOLUME : "2804"
PAGE   : "78-89"
YEAR   : "1996"
TOPKEY : "Coriolis-SMEI"
ABS    : "The Solar Mass Ejection Imager (SMEI) experiment is designed to detect and measure transient plasma features in the heliosphere, including coronal mass ejections, shock waves, and structures such as streamers which corotate with the Sun. SMEI will provide measurements of the propagation of solar plasma clouds and high-speed streams which can be used to forecast their arrival at Earth from one to three days in advance. The white light photometers on the HELIOS spacecraft demonstrated that visible sunlight scattered from the free electrons of solar ejecta can be sensed in interplanetary space with an electronic camera baffled to remove stray background light. SMEI promises a hundred-fold improvement over the HELIOS data, making possible quantitative studies of mass ejections. SMEI measurements will help predict the rate of energy transfer into the Earth's magnetospheric system. By combining SMEI data with solar, interplanetary and terrestrial data from other space and ground-based instruments, it will be possible to establish quantitative relationships between solar drivers and terrestrial effects. SMEI consists of three cameras, each imaging a 60 degree(s) &times; 3 degree(s) field of view for a total image size of 180 degree(s) &times; 3 degree(s). As the satellite orbits the earth, repeated images are used to build up a view of the entire heliosphere."

---
MARKER : "1996_isa_42_17"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Buffington, A., Hick, P., Kahler, S.W., Keil, S.L., Simnett, G., Webb, D.F."
TITLE  : "The Solar Mass Ejection Imager"
CTITLE : "Proc. 42^th International Instrument Symp. of the Instrument Society of America, San Diego, 1996"
PAGE   : "17-23"
YEAR   : "1996"
TOPKEY : "Coriolis-SMEI"
ABS    : "We are designing a Solar Mass Ejection Imager (SMEI) capable of observing Thomson-scattered signals from transient density features in the heliosphere from a spacecraft situated near 1 AU. The imager is designed to trace features, which include coronal mass ejections, corotating structures and shock waves, to elongations greater than 90&deg; from the Sun. An imager at Earth could allow up to three days warning of the arrival of a mass ejection from the Sun. The instrument can be regarded as a progeny of the heliospheric imaging capability shown possible by the zodiacal light photometers of the HELIOS spacecraft. The instrument we are designing must utilize one of the most advanced baffle systems yet devised to eliminate sunlight from its wide field of view. In addition, the instrument must couple the wide field of view to a CCD camera so that the small percentage variations of the Thomson-scattered signals can be detected relative to a much brighter zodiacal light and stellar background."

---
MARKER : "1996_aspcs_95_167"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Webb, D.F., Jackson, B.V., Hick, P."
TITLE  : "Geomagnetic storms and heliospheric CMEs as viewed from HELIOS"
EDITOR : "Balasubramaniam, K.S., Keil, S.L., Smartt, R.N."
CTITLE : "Solar drivers of interplanetary and terrestrial disturbances"
SERIAL : "ASP Conf. Series"
VOLUME : "95"
PAGE   : "167-170"
YEAR   : "1996"
TOPKEY : "Helios photometers"
ABS    : "In recent years, several solar wind signatures considered as proxies for Coronal Mass Ejections (CMEs), such as periods of bidirectional electron flows following fast shocks, have been associated with large, sporadic geomagnetic storms. To study the characteristics of CMEs that are associated with storms, we examine a subset of the database of CMEs directly observed by the HELIOS white light photometers from 1975-1983. The important advantage of the HELIOS data set is that it provides a unique identification of the extent of enhanced plasma density associated with each CME and the general time of its passage by the spacecraft. We selected those CMEs which enveloped the HELIOS spacecraft in the ecliptic plane when it was within about 30 degrees ecliptic longitude east or west of the Sun-Earth line; there are about 40 CMEs in this sample. The photometer data are used to estimate such characteristics of the heliopsheric CMEs as their speeds, durations, scale sizes and masses.  HELIOS in-situ magnetic field and plasma data are used to identify periods of bidirectionally streaming electron and ion flows, magnetic 'clouds' and shocks during the intervals of CME passage by the spacecraft. When appropriate, these signatures are compared with similar events identified previously in the ISEE-3 (1978-1982) and IMP-8 data in Earth orbit at 1 AU. We will present preliminary results of this analysis pertaining to the characteristics of CMEs associated with storms."

---
MARKER : "1996_aspcs_95_158"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Keil, S.L., Altrock, R.C., Kahler, S.W., Jackson, B.V., Buffington, A., Hick, P., Simnett, G., Eyles, C., Webb, D.F., Anderson, P."
TITLE  : "The Solar Mass Ejection Imager (SMEI): development and use in space weather forecasting"
EDITOR : "Balasubramaniam, K.S., Keil, S.L., Smartt, R.N."
CTITLE : "Solar drivers of interplanetary and terrestrial disturbances"
SERIAL : "ASP Conf. Series"
VOLUME : "95"
PAGE   : "158-165"
YEAR   : "1996"
TOPKEY : "Coriolis-SMEI"
ABS    : "The Solar Mass Ejection Imager (SMEI) experiment will measure plasma features traversing the heliosphere, including coronal mass ejections (CMEs), shock waves, and structures such as streamers which corotate with the Sun. SMEI will measure propagation characteristics of these features providing one to three day forecasts of their arrival at Earth. The white light photometers on the HELIOS spacecraft demonstrated that electronic cameras, baffled to remove scattered light, can sense visible sunlight scattered from the free electrons of solar ejecta propagating through interplanetary space. SMEI promises a hundred-fold improvement over HELIOS, making possible quantitative studies of mass ejections. SMEI is highly complementary to other satellite missions, the Global Geospace Program (GGS), and the National Space Weather Program. When coordinated with the imaging and in situ experiments on SOHO, TRACE, WIND, ULYSSES, and SXI. SMEI will greatly enhance the GGS program by predicting the rate of energy transfer from transient interplanetary disturbances into the Earth's magnetospheric system being monitored by GGS satellites. The SMEI data will assist researchers in establishing quantitative relationships between solar drivers and terrestrial effects."

---
MARKER : "1996_aspcs_95_358"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Hick, P., Jackson, B.V., Altrock, R.C., Slater, G., Henry, T."
TITLE  : "The coronal temperature structure and the current sheet"
EDITOR : "Balasubramaniam, K.S., Keil, S.L., Smartt, R.N."
CTITLE : "Solar drivers of interplanetary and terrestrial disturbances"
SERIAL : "ASP Conf. Series"
VOLUME : "95"
PAGE   : "358-365"
YEAR   : "1996"
TOPKEY : "corona"
ABS    : "We explore the large-scale temperature structure of the low corona using synoptic temperature maps, derived from the intensity ratio of the green (Fe XIV) and red (Fe X) coronal lines as observed at the National Solar Observatory/Sacramento Peak, and temperature maps derived from the Al0.1 and AlMgMn filter intensity ratio measured by the Yohkoh/SXT instrument. The red/green intensity ratio is sensitive to coronal plasma with temperatures in the range of 1-2 MK and is therefore useful for studying the 'quiet' corona. The Yohkoh/SXT filter ratio covers a much wider range of coronal temperature (&gt; 1 MK) and, in particular, is sensitive to the high temperatures (&gt; 3 MK) commonly observed above active regions. We use the temperature maps to study the evolution of the large-scale coronal temperature distribution, in particular in relation to the large-scale magnetic field, as given by the 'source surface' maps derived from the Stanford potential field model. We find that the large-scale high-temperature features follow the heliospheric current sheet remarkably well, especially when the current sheet is stable over several rotations."

---
MARKER : "1996_aspcs_95_470"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Hick, P., Jackson, B.V."
TITLE  : "The influence of active regions on IPS measurements near 1 AU"
EDITOR : "Balasubramaniam, K.S., Keil, S.L., Smartt, R.N."
CTITLE : "Solar drivers of interplanetary and terrestrial disturbances"
SERIAL : "ASP Conf. Series"
VOLUME : "95"
PAGE   : "470-471"
YEAR   : "1996"
TOPKEY : "IPS"
ABS    : "Interplanetary scintillation (IPS) measurements can be used to explore the heliospheric density structure. We have used observations of the IPS 'disturbance factor' g near 1 AU, obtained with the Cambridge (UK) array, to investigate the solar source of low-level IPS disturbances. Using a ballistic mapping technique we construct synoptic maps representing the large-scale enhancements of the <i>g</i> factor. By comparing these synoptic maps with near-solar surface data, such as synoptic maps of coronal x-ray emission obtained with the Yohkoh/SXT instrument, maps of coronal green line emission obtained with the Sac. Peak Evans facility, and maps of the heliospheric current sheet as derived from the Stanford potential field model, we find that active regions contribute significantly to the small-scale (~200 km) density variations (as measured by the g factor), which cause the IPS near 1 AU. Since the level of density variations is related to the heliospheric density itself we conclude that active regions are a significant factor in modulating the solar wind and contribute to the solar wind mass output."

---
MARKER : "1996_sw8_536"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Buffington, A., Hick, P., Kahler, S.W., Altrock, R.C., Gold, R.E., Webb, D.F."
TITLE  : "The Solar Mass Ejection Imager"
EDITOR : "Winterhalter, D., Gosling, J.T., Habbal, S.R., Kurth, W.S., Neugebauer, M."
CTITLE : "Solar Wind Eight"
SERIAL : "AIP Conf. Proc."
VOLUME : "382"
PAGE   : "536-539"
YEAR   : "1996-07"
DOI    : "10.1063/1.51509"
TOPKEY : "Coriolis-SMEI"
ABS    : "We are designing a Solar Mass Ejection Imager (SMEI) capable of observing Thomson-scattered signals from transient density features in the heliosphere from a spacecraft situated near 1 AU. The imager is designed to trace these features, which include coronal mass ejections, corotating structures and shock waves, to elongations greater than 90&deg; from the Sun. The instrument may be regarded as a progeny of the heliospheric imaging capability shown possible by the zodiacal light photometers of the HELIOS spacecraft. The instrument we are designing would make more effective use of in situ solar wind data from spacecraft in the vicinity of the imager by extending their observations to the surrounding environment. An imager in Earth orbit could allow up to three days warning of the arrival of a mass ejection from the Sun."

---
MARKER : "1996_sw8_169"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Hick, P., Jackson, B.V., Altrock, R.C."
TITLE  : "Coronal synoptic temperature maps derived from the Fe XIV/Fe X intensity ratio"
EDITOR : "Winterhalter, D., Gosling, J.T., Habbal, S.R., Kurth, W.S., Neugebauer, M."
CTITLE : "Solar Wind Eight"
SERIAL : "AIP Conf. Proc."
VOLUME : "382"
PAGE   : "169-172"
YEAR   : "1996-07"
DOI    : "10.1063/1.51467"
TOPKEY : "corona"
ABS    : "The large-scale temperature structure of the low corona is investigated using synoptic temperature maps, derived from the intensity ratio of the green (Fe XIV) and red (Fe X) coronal lines as observed at the National Solar Observatory/Sacramento Peak. This intensity ratio is sensitive to coronal plasma with temperatures of 1-2 MK, a range of temperatures ususally associated with the quiet corona. The synoptic maps indicate an association between high coronal temperature and the large-scale magnetic field. A comparison with Stanford 'source surface' synoptic maps shows that, especially when the heliospheric current sheet is stable over several rotations, the large-scale high-temperature features follow the current sheet remarkably well. For recent Carrington rotations, temperaute maps are available for four heights between 1.15 and 1.45 R_sun. For these maps the correspondence with the current sheet (calculated at 2.5 R_sun) improves with height. Discrepancies between temperature structure and magnetic structure appear to be largest when the magnetic structure changes rapidly from rotation to rotation."

---
MARKER : "1996_sw8_461"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Hick, P., Jackson, B.V."
TITLE  : "Evidence of active region imprints on the solar wind structure"
EDITOR : "Winterhalter, D., Gosling, J.T., Habbal, S.R., Kurth, W.S., Neugebauer, M."
CTITLE : "Solar Wind Eight"
SERIAL : "AIP Conf. Proc."
VOLUME : "382"
PAGE   : "461-464"
YEAR   : "1996-07"
DOI    : "10.1063/1.51498"
TOPKEY : "IPS"
ABS    : "A common descriptive framework for discussing the solar wind structure in the inner heliosphere uses the global magnetic field as a reference: low density, high velocity solar wind emanates from open magnetic fields, with high density, low speed solar wind flowing outward near the current sheet. In this picture, active regions, underlying closed magnetic field structures in the streamer belt, leave little or no imprint on the solar wind. We present evidence from interplanetary scintillation measurements of the 'disturbance factor' g that active regions play a role in modulating the solar wind and possibly contribute to the solar wind mass output. Hence we find that the traditional view of the solar wind, though useful in understanding many features of solar wind structure, is oversimplified and neglects important aspects of solar wind dynamics."

---
MARKER : "1996_asr_17_235"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Altrock, R.C., Hick, P., Jackson, B.V., Hoeksema, J.T., Zhao, X.P., Slater, G., Henry, T.W."
TITLE  : "Solar coronal structure: A comparison of NSO/SP ground-based coronal emission line intensities and temperatures with Yohkoh SXT and WSO magnetic data"
EDITOR : "Culhane, J.L., Hiei, E."
CTITLE : "Solar flare, coronal and heliospheric dynamics"
SERIAL : "Adv. Space Res."
VOLUME : "17 (4/5)"
PAGE   : "235-238"
YEAR   : "1996"
DOI    : "10.1016/0273-1177(95)00576-Z"
TOPKEY : "corona"
ABS    : "The large-scale structure of the solar corona is investigated using synoptic maps produced from Fe XIV (530.3 nm), Fe X (637.4 nm) and Ca XV (569.4 nm) data obtained at NSO/SP, Yohkoh/SXT X-ray data and Wilcox Solar Observatory (WSO) `source surface' maps. We find that the Fe XIV data are an excellent proxy for spatially-averaged Yohkoh/SXT data. Isolated emission features and large-scale structures are nearly identical in SXT and Fe XIV maps. In addition, coronal holes and other low-emission regions are very similar. Synoptic temperature maps, calculated from the Fe X/Fe XIV ratio, show a tendency for the highest temperatures to occur where the large-scale magnetic fields change polarity at high latitudes (cf. /1/), while lower-latitude features, including active regions, have lower apparent temperatures. Regions of enhanced temperature generally follow the heliospheric current sheet (HCS) as defined by the WSO maps. Further, emission in Ca XV (formed at T&asymp;3 MK), generally occurs only over low-latitude regions that are bright in both Fe X (T&asymp;1 MK) and Fe XIV (T&asymp;2 MK). Thus, there is evidence for low (&asymp;1 MK), moderate (&asymp; 2 MK) and high (&asymp;3 MK) temperatures in close proximity in the low corona."

---
MARKER : "1996_asr_17_311"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Hick, P., Jackson, B.V, Altrock, R., Woan, G., Slater, G."
TITLE  : "IPS observations of heliospheric density structures associated with active regions"
EDITOR : "Culhane, J.L., Hiei, E."
CTITLE : "Solar flare, coronal and heliospheric dynamics"
SERIAL : "Adv. Space Res."
VOLUME : "17 (4/5)"
PAGE   : "311-314"
YEAR   : "1996"
DOI    : "10.1016/0273-1177(95)00591-2"
TOPKEY : "IPS"
ABS    : "Interplanetary scintillation (IPS) measurements of the 'disturbance factor' g, obtained with the Cambridge (UK) array can be used to explore the heliospheric density structure. We have used these data to construct synoptic (Carrington) maps, representing the large-scale enhancements of the g-factor in the inner heliosphere. These maps emphasize the stable corotating, rather than the transient heliospheric density enhancements. We have compared these maps with Carrington maps of Fe XIV observations (NSO, Sacramento Peak) and maps based on Yohkoh/SXT X-ray observations. Our results indicate that the regions of enhanced g tend to map to active regions rather than the current sheet. The implication is that active regions are the dominant source of the small-scale (&asymp;200 km) density variations present in the quiet solar wind."

---
MARKER : "1996_adv_space_res_17_115"
TYPE   : "in_proceedings"
AUTHOR : "Rompolt, B., Svestka, Z."
TITLE  : "Flare-like dynamic phenomena"
EDITOR : "Culhane, J.L., Hiei, E."
CTITLE : "Solar flare, coronal and heliospheric dynamics, COSPAR 30, 11-21 July 1994, Hamburg, Germany"
SERIAL : "Adv. Space Res."
VOLUME : "17 (4-5)"
PAGE   : "115-124"
YEAR   : "1996-00"
DOI    : "10.1016/0273-1177(95)00552-P"

---
MARKER : "1966_joso_ann_rep_135"
TYPE   : "in_book"
AUTHOR : "Svestka, Z."
TITLE  : "Coronal phenomena associated with flares"
CTITLE : "JOSO Annual Report"
PAGE   : "135-140"
YEAR   : "1996-00"

---
MARKER : "1995_colleferro"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Buffington, A., Hick, P., Kahler, S.W., Keil, S.L., Altrock, R.C., Simnett, G.M., Webb, D.F."
TITLE  : "The Solar Mass Ejection Imager"
EDITOR : "Pecorella, W., Mura, R."
CTITLE : "Proc. Workshop in Colleferro, Italy (12-13 Oct, 1995) on Small mission opportunities and the scientific community"
YEAR   : "1995"
REMARK : "submitted, but never published?"
TOPKEY : "Coriolis-SMEI"

---
MARKER : "1995_solar_phys_161_331"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Svestka, Z., Farnik, F., Hudson, H.S., Uchida, Y., Hick, P., Lemen, J.R."
TITLE  : "Large scale active coronal phenomena in Yohkoh SXT images, I. Post-flare giant arches rising with constant speed"
SERIAL : "Solar Phys."
VOLUME : "161 (2)"
PAGE   : "331-363"
YEAR   : "1995-11"
DOI    : "10.1007/BF00732074"
TOPKEY : "post-flare arch"
ABS    : "The authors have found several occurrences of slowly rising giant arches in Yohkoh images. These are similar to the giant post-flare arches previously discovered by SMM instruments in the 80s. However, the authors see them now with 3-5 times better spatial resolution and can recognize well their loop-like structure. As a rule, these arches follow eruptive flares with gradual soft X-ray bursts, and rise with speeds of 1.1-2.4 km s^-1 which keep constant for ~5 to 24 hours, reaching altitudes up to 250 000 km above the solar limb. These arches differ from post-flare loop systems by their (much higher) altitudes, (much longer) lifetimes, and (constant) speed of growth. One event appears to be a rise of a transequatorial interconnecting loop. In the event of 21-22 February 1992 one can see both the loop system, rising with a gradually decreasing speed to an altitude of 120 000 km, and the arch, emerging from behind the loops and continuing to rise with a constant speed for many more hours up to 240 000 km above the solar limb. In the event of 2-3 November 1991 three subsequent rising large-scale coronal systems can be recognized: first a fast one with speed increasing with altitude and ceasing to be visible at about 300 000 km. This most probably shows the X-ray signature of a coronal mass ejection (CME). A second one, with gradually decreasing speed, might represent very high rising flare loops. A third one continues to rise slowly with a constant speed up to 230 000 km (and up to 285 000 km after the speed begins to decay), and this is the giant arch. This event, including an arch revival on November 4-5, is very similar to rising giant arches observed by the SMM on 6-7 November 1980. Other events of this kind were observed on 27-28 April 1992, 15 March 1993, and 4-6 November 1993, all seen above the solar limb, where it is much easier to identify them. The temperature in the brightest part of the arch of 2-3 November 1991 was increasing with its altitude, from 2 to 4&times;10^6 K, which seems to be an effect of slower cooling at lower densities. Under an assumption of line-of-sight thickness of 50000 km, the emission measure indicates densities from 1.1&times;10^10 cm^-3 at an altitude of 150 000 km to 1.0&times;10^9 cm^-3 at 245 000 km 11.5 hours later. It appears that the arch is composed of plasma of widely different temperatures, and that hot plasma rises faster than the cool component. Thus the whole arch expands upward, and its density gradient increases with time, which explains why Yohkoh images show only the lowest and coolest parts of the expanding structure. The whole arch may represent an energy in excess of 10^31 erg, and more if conduction contributes to the arch cooling. The authors suggest that the rise of the arch is initiated by a CME which removes the magnetic field and plasma in the upper corona, and the coronal structures remaining below this cavity begin to expand into the 'vacuum' left behind the CME. However, they are unable to explain why the speed of rise stays constant for so many hours."

---
MARKER : "1995_solar_phys_160_53"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "On ‘the Solar Flare Myth’ postulated by Gosling"
SERIAL : "Solar Phys."
VOLUME : "160 (1)"
PAGE   : "53-56"
YEAR   : "1995-08"
DOI    : "10.1007/BF00679093"

---
MARKER : "1995_solar_phys_159_403"
TYPE   : "in_journal"
AUTHOR : "Solanki, S.K., Svestka, Z."
TITLE  : "Book reviews"
SERIAL : "Solar Phys."
VOLUME : "159 (2)"
PAGE   : "403-404"
YEAR   : "1995-07"
DOI    : "10.1007/BF00686542"
REMARK : "book review"

---
MARKER : "1995_jpl_de403"
TYPE   : "tech. report"
AUTHOR : "Standish, E.M., Newhall, X.X., Williams, G.G., Folkner, W.M."
TITLE  : "JPL Planetary and Lunar Ephemerides, DE403/LE403"
PAGE   : "(27 pages)"
TOPKEY : "ephemeris"
YEAR   : "1995-05"

---
MARKER : "1995_esa_sp_373_199"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Hick, P."
TITLE  : "Three dimensional reconstruction of coronal mass ejections"
EDITOR : "Hunt, J.J."
CTITLE : "3^rd SOHO Workshop on Solar dynamic phenomena and solar wind consequences"
SERIAL : "ESA SP"
VOLUME : "373"
PAGE   : "199-202"
PUBLISH: "ESTEC, Noordwijk, Netherlands"
YEAR   : "1995"
TOPKEY : "Helios photometers"
ABS    : "We use computer assisted tomography (CAT) techniques to reconstruct the three-dimensional shape of coronal mass ejections in the interplanetary medium. Both the Helios 2 spacecraft zodiacal-light photometers and the Solwind coronagraph measure changes in Thomson scattering of sunlight from electrons. Here we use the technique from near-perpendicular Solwind and Helios views to determine the density of a mass ejection which left the solar surface on 24 May 1979. The coronagraph and the Helios perspective views are not simultaneous; the Solwind observations extend outward to sky plane distances of only 10 R_sun, whereas the Helios 16&deg; photometer observes to as close as 17 R<sub>sun</sub> from the Sun. However, by assuming outward radial expansion and that the CMEs have the same speed everywhere at the same height, we obtain a solution. The analyses show that CMEs are extensive three dimensional structures - the CME of 24 May appears approximately shell-like in three dimensions.
"

---
MARKER : "1995_grl_22_643"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Hick, P., Jackson, B.V, Rappoport, S., Woan, G., Slater, G., Strong, K., Uchida, Y."
TITLE  : "Synoptic IPS and Yohkoh soft X-ray observations"
SERIAL : "Geophys. Res. Lett."
VOLUME : "22 (5)"
PAGE   : "643-646"
YEAR   : "1995-03"
DOI    : "10.1029/95GL00011"
TOPKEY : "IPS, X-rays"
ABS    : "We have examined the relationship between solar wind speed and electron density fluctuations on scale sizes around 100 km in the heliocentric distance range of 0.3 to 0.8 AU using interplanetary scintillation (IPS) data obtained at the Solar-Terrestrial Environment Laboratory. The solar wind properties derived from the IPS data are biased by line of sight integration through a three-dimensional structured solar wind. Therefore we have applied a computer-assisted tomography (CAT) method to deconvolve the line of sight integration and reconstruct the solar wind structure. The analysis was made for the solar wind speed V and electron density fluctuations &delta;N_e in the solar activity minimum phase when high-speed regions are separated from an equatorial low-speed region by a sharp velocity gradient. From results of the CAT analysis we derived the best fit power law relation of &delta;N_e~V_&minus;&gamma; with &gamma;=0.5&plusmn;0.15, indicating that fractional density fluctuations &delta;N_e/N_e in the high-speed wind are larger than those in the low-speed wind. Combining this relation with results of previous workers [Coles et al., 1995; Manoharan, 1993; Celnikier t al., 1987; Jackson t al., 1998], we suggest that the fractional density fluctuation level of the high-speed wind evolves with heliocentric distance."

---
MARKER : "1995_adv_space_res_16_27"
TYPE   : "in_proceedings"
TITLE  : "A comparison of solar activity during the decline of several solar cycles"
AUTHOR : "Svestka, Z."
SERIAL : "Adv. Space Res."
VOLUME : "16 (9)"
PAGE   : "27-36"
YEAR   : "1995-00"
DOI    : "10.1016/0273-1177(95)00311-2"

---
MARKER : "1994_aasup_108_279"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Buffington, A., Hick, P., Kahler, S.W., Webb, D.F."
TITLE  : "A spaceborne near-Earth asteroid detection system"
SERIAL : "Astron. Astrophys. Suppl. Ser."
VOLUME : "108"
PAGE   : "279-285"
YEAR   : "1994-12"
TOPKEY : "asteroids"
ABS    : "We have designed a Solar Mass Ejection Imager (SMEI) to image transient heliospheric features from Earth orbit over the entire sky every 90 minutes. The instrument is designed to detect changes on this time scale in the signals from sunlight Thomson-scattered from electrons at a brightness level of tenth magnitude per square degree of sky. We explore the possibility of using such an instrument to detect asteroids passing near the Earth. We estimate that SMEI will detect at least 13 asteroids per year over ~12m in radius."

---
MARKER : "1994_solar_phys_155_121"
TYPE   : "in_journal"
AUTHOR : "Kallenrode, M.-B., Svestka, Z."
TITLE  : "The participation of nuclei in type-III-related electron streams"
SERIAL : "Solar Phys."
VOLUME : "155 (1)"
PAGE   : "121-148"
YEAR   : "1994-11"
DOI    : "10.1007/BF00670735"

---
MARKER : "1994_solar_phys_152_393"
TYPE   : "in_journal"
AUTHOR : "Heinzel, P., Karlicky, M., Kotrc, P., Svestka, Z."
TITLE  : "On the occurrence of blue asymmetry in chromospheric flare spectra"
SERIAL : "Solar Phys."
VOLUME : "152 (2)"
PAGE   : "393-408"
YEAR   : "1994-07"
DOI    : "10.1007/BF00680446"

---
MARKER : "1994_solar_phys_152_505"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Slow-mode oscillations of large-scale coronal loops"
SERIAL : "Solar Phys."
VOLUME : "152 (2)"
PAGE   : "505-508"
YEAR   : "1994-07"
DOI    : "10.1007/BF00680454"

---
MARKER : "1994_solar_phys_151_203"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Book review"
SERIAL : "Solar Phys."
VOLUME : "151 (1)"
PAGE   : "203"
YEAR   : "1994-04"
DOI    : "10.1007/BF00654094"
REMARK : "book review"

---
MARKER : "1994_solar_phys_149_363"
TYPE   : "in_journal"
AUTHOR : "Smith, K.L., Strong, K.T., Svestka, Z., McCabe, M.K."
TITLE  : "X-ray observations of a major eruptive flare behind the limb"
SERIAL : "Solar Phys."
VOLUME : "149 (2)"
PAGE   : "363-380"
YEAR   : "1994-02"
DOI    : "10.1007/BF00690622"

---
MARKER : "1994_pltr_94_2040"
TYPE   : "report"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Webb, D.F., Hick, P., Nelson, J.L."
TITLE  : "Catalog of Helios 90^deg photometer events"
PUBLISH: "Phillips Lab., Hanscom, MA (PL-TR-94-2040 Scientific Report No. 4)"
YEAR   : "1994-02"
URL    : "http://www.stormingmedia.us/41/4149/A414972.html"
TOPKEY : "Helios photometers"
ABS    : "Helios spacecraft were launched into solar orbits in December 1974 and January 1976. Each spacecraft contained three zodiacal light photometers intended to measure the distribution of dust in the interplanetary medium between the Sun and the Earth. Residual brightness variations were evident after the zodiacal light and stellar contributions had been removed from the photometer data. These variations are now known to have been caused primarily by transient plasma clouds propagating through the inner heliosphere. About 2/3 of these were caused by coronal mass ejections and about 1/4 by corotating structures. We have used specific criteria to select and identify these plasma events in the data from the Helios photometers which are pointed at the ecliptic poles. This process is now complete and we are making these data available to the scientific community. This document is a catalog of the Helios 90 deg photometer events which we have identified. In the following text we describe the pertinent characteristics of the zodiacal light experiment, the methods used to select, identify and classify the 90 deg events, and the details of the catalog structure. A comprehensive bibliography of all published papers involving analyses of the Helios photometer plasma observations and the zodiacal light calibration is also included."

---
MARKER : "1994_asr_14_135"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Hick, P., Jackson, B.V."
TITLE  : "Solar wind mass and momentum flux variations at 0.3 AU"
EDITOR : "Gabriel, A."
CTITLE : "The structure and physical properties of the quiet solar corona"
SERIAL : "Adv. Space Res."
VOLUME : "14 (4)"
PAGE   : "135-138"
YEAR   : "1994"
DOI    : "10.1016/0273-1177(94)90172-4"
TOPKEY : "Helios photometers, IPS"
ABS    : "In the past we have used electron Thomson scattering brightness observations, obtained with the zodiacal-light photometers on board the spacecraft Helios 1 and Helios 2, to study the global density structure of the quiet corona and inner heliosphere (&gt; 17 solar radii). This was done by means of a comparison of synoptic maps based on these Thomson scattering observations and synoptic maps based on other solar/heliospheric data, such as IPS velocity, K-coronameter brightness and magnetic source surface data. In this paper we continue this approach by combining the Helios Thomson scattering maps (which provide density information) with IPS solar wind velocity maps to map out variations in mass and momentum flux of the solar wind as a function of latitude and phase of the solar cycle. The method used to construct the Helios and IPS synoptic maps emphasizes the global, persistent (as opposed to transient) structures, and thus can be viewed as approximating conditions in the quiet corona and inner heliosphere."

---
MARKER : "1994_iau_coll_144_243"
TYPE   : "in_proceedings"
AUTHOR : "Svestka, Z., Farnik, F."
TITLE  : "Large-scale coronal structures associated with solar activity"
EDITOR : "Rusin, V., Heinzel, P., Vial, J.-C."
CTITLE : "Proc. 144^th IAU Coll. on Solar coronal structures"
PLACE  : "Lomnical, Slovakia, 10-14 September 1993"
PAGE   : "243-250"
YEAR   : "1994-00"
PUBLISH: "VEDA Publ. House of the Slovak Academy of Sciences"
URL    : "http://adsabs.harvard.edu/abs/1994scs..conf..243S"

---
MARKER : "1993_solar_phys_148_177"
TYPE   : "in_journal"
AUTHOR : "Švestka, Z."
TITLE  : "Book review"
SERIAL : "Solar Phys."
VOLUME : "148 (1)"
PAGE   : "177-178"
YEAR   : "1993-11"
DOI    : "10.1007/BF00675544"
REMARK : "book review"

---
MARKER : "1993_asr_13_71"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Webb, D.F., Jackson, B.V., Hick, P., Schwenn, R., Bothmer, V., Reames, D."
TITLE  : "Comparison of CMEs, magnetic clouds, and bidirectionally streaming proton events in the heliosphere using Helios data"
EDITOR : "Pick, M., Machado, M.E."
CTITLE : "Fundamental problems in solar activity"
SERIAL : "Adv. Space Res."
VOLUME : "13 (9)"
PAGE   : "71-74"
YEAR   : "1993"
DOI    : "10.1016/0273-1177(93)90459-O"
TOPKEY : "Helios photometers"
ABS    : "Coronal Mass Ejections (CMEs) are large, energetic expulsions of mass and magnetic fields from the Sun; they can significantly affect large volumes of the heliosphere and appear to be a key cause of geomagnetic storms. We have compiled a list of all significant CMEs detected by the HELIOS white light photometers from 1975-1982. We are studying the characteristics of these CMEs, and present preliminary results of their associations with in-situ features, especially magnetic 'clouds' and periods of bidirectionally streaming ions, two classes of structures considered indicative of interplanetary loops.  Advantages of this data set include reliable association in the interplanetary medium of the white light CME plasma with the in-situ features, and observations of a large number of events over a long time base."

---
MARKER : "1993_asr_13_43"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V, Hick, P., Webb, D.F."
TITLE  : "Co-rotating structures of the inner heliosphere from Helios photometer and in-situ data"
EDITOR : "Pick, M., Machado, M.E."
CTITLE : "Fundamental problems in solar activity"
SERIAL : "Adv. Space Res."
VOLUME : "13 (9)"
PAGE   : "43-46"
YEAR   : "1993"
DOI    : "10.1016/0273-1177(93)90455-K"
TOPKEY : "Helios photometers"
ABS    : "We have compiled a list of all major co-rotating structures in the inner heliosphere detected by the white light photometers of both HELIOS spacecraft from 1975?1982.  We compare the three-dimensional extents of these remotely-sensed structures over their times of observation. We pay particular attention to the spatial extent of these structures and their variability. We can measure the in-situ characteristics of the subset of structures as they envelop the spacecraft. The advantages of this data set include the association of the three-dimensional extent of these co-rotating structures with in-situ observations of the same features."

---
MARKER : "1993_solar_phys_148_359"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Howard, R.A."
TITLE  : "A CME mass distribution derived from SOLWIND coronagraph observations"
SERIAL : "Solar Phys."
VOLUME : "148"
PAGE   : "359-370"
YEAR   : "1993-12"
DOI    : "10.1007/BF00645095"
TOPKEY : "coronal mass ejections"
ABS    : "Using estimates of the masses of nearly 1000 CMEs observed by SOLWIND from Howardet al. (1985), we re-plot the numbers of CMEs as a function of CME mass on a log-linear plot. The plot is significant in that it shows a linear trend over more than a decade of CME masses. The plot indicates a simple form for the distribution of the CME masses and allows an easy determination of the total mass ejected into the solar wind in the form of CMEs. We find that approximately 16% of the solar wind at solar maximum can be comprised of CME mass. There is no indication that the numbers of low-mass CMEs increase in number above the trend set by the more massive ones. Specifically, there is no increase in the numbers of small CMEs such that the whole of the solar wind can be comprised of them."

---
MARKER : "1993_solar_phys_146_313"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Farnik, F., Hick, P., Svestka, Z."
TITLE  : "Responses of large-scale coronal structures to chromospheric activity"
SERIAL : "Solar Phys."
VOLUME : "146 (2)"
PAGE   : "313-330"
YEAR   : "1993-08"
DOI    : "10.1007/BF00662016"
TOPKEY : "chromosphere"
ABS    : "We have followed the transit of two active regions across the western solar limb during June 29 through July 2, 1980, as imaged in 3.5-16 keV X-rays by HXIS aboard the SMM. During frequent brightenings of large-scale coronal structures, hard X-ray emission in the 11-16 keV energy band was recorded up to altitudes of 76,000 km. Soft X-rays could be seen in excess of 250,000 km altitude above the photospheric active region. Many X-ray brightenings low in the corona in the active regions were followed by enhancements high in the corona in the large-scale coronal structures. Although subsequent enhancements rarely appeared in the same position, similar portions of the corona brightened intermittently, indicating that the general configuration of the coronal structures above the active regions did not change much, in spite of the frequent energy inputs. These inputs were of two kinds: nonthermal, with very fast response at high coronal altitudes within seconds or tens of seconds, and thermal, with a delay of several minutes. The nonthermal response is short-lived, reflecting the time profile of the primary source; the thermal response is more gradual and longer lasting than the primary source. In some enhancements of large-scale coronal structures both these kinds of response occur and can be clearly recognized. There are also active-region brightenings without any response in the high corona and, vice versa, high-corona brightenings without any obvious primary source; in the latter case, it is likely that the source was hidden behind the limb."

---
MARKER : "1993_solar_phys_146_343"
TYPE   : "in_journal"
AUTHOR : "Šimberova, S., Karlicky, M., Svestka, Z."
TITLE  : "An analysis of Skylab X-ray pictures of a giant coronal arch"
SERIAL : "Solar Phys."
VOLUME : "146 (2)"
PAGE   : "343-356"
YEAR   : "1993-08"
DOI    : "10.1007/BF00662018"

---
MARKER : "1993_solar_phys_143_401"
TYPE   : "in_journal"
AUTHOR : "de Jager, C., Howard, R.F., Svestka, Z."
TITLE  : "Book reviews"
SERIAL : "Solar Phys."
VOLUME : "143 (2)"
PAGE   : "401"
YEAR   : "1993-02"
DOI    : "10.1007/BF00646497"
REMARK : "editorial"

---
MARKER : "1993_solar_phys_143_vii"
TYPE   : "in_journal"
AUTHOR : "de Jager, C., Howard, R.F., Svestka, Z."
TITLE  : "Editorial"
SERIAL : "Solar Phys."
VOLUME : "143 (1)"
PAGE   : "vii"
YEAR   : "1993-01"
DOI    : "10.1007/BF00619092"
REMARK : "editorial"

---
MARKER : "1992_solar_phys_139_405"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z., Smith, K.L., Strong, K.T."
TITLE  : "X-ray observations of limb flare loops and post-flare coronal arch"
SERIAL : "Solar Phys."
VOLUME : "139 (2)"
PAGE   : "405-408"
YEAR   : "1992-06"
DOI    : "10.1007/BF00159162"

---
MARKER : "1992_solar_phys_138_189"
TYPE   : "in_journal"
AUTHOR : "Poletto, G., Svestka, Z."
TITLE  : "The birth of giant post-flare arches"
SERIAL : "Solar Phys."
VOLUME : "138 (1)"
PAGE   : "189-199"
YEAR   : "1992-03"
DOI    : "10.1007/BF00146203"

---
MARKER : "1992_solar_phys_137_v"
TYPE   : "in_journal"
AUTHOR : "de Jager, C., Svestka, Z., Howard, R.F."
TITLE  : "Editorial"
SERIAL : "Solar Phys."
VOLUME : "137 (1)"
PAGE   : "v"
YEAR   : "1992-01"
DOI    : "10.1007/BF00146571"
REMARK : "editorial"

---
MARKER : "1992_lnp_399"
TYPE   : "proceedings"
EDITOR : "Svestka, Z., Jackson, B.V., Machado, M.E."
TITLE  : "Eruptive solar flares, Proc. IAU Coll. No. 133, Iguazú, Argentina, 2-6 August 1991"
SERIAL : "Lecture Notes in Physics"
VOLUME : "399"
PAGE   : "(xiv+409 pages)"
YEAR   : "1992-00"
PUBLISH: "Springer, Berlin"
DOI    : "10.1007/3-540-55246-4"

---
MARKER : "1992_lnp_399_1"
TYPE   : "in_proceedings"
AUTHOR : "Svestka, Z., Cliver, E.W."
TITLE  : "History and basic characteristics of eruptive flares"
CTITLE : "Eruptive solar flares"
EDITOR : "Svestka, Z., Jackson, B.V., Machado, M.E."
SERIAL : "Lecture Notes in Physics"
VOLUME : "399"
PAGE   : "1-11"
YEAR   : "1992-00"
DOI    : "10.1007/3-540-55246-4_70"

---
MARKER : "1992_lnp_399_221"
TYPE   : "in_proceedings"
AUTHOR : "Svestka, Z., Simberova, S."
TITLE  : "A giant post-flare coronal arch observed by Skylab"
CTITLE : "Eruptive solar flares"
EDITOR : "Svestka, Z., Jackson, B.V., Machado, M.E."
SERIAL : "Lecture Notes in Physics"
VOLUME : "399"
PAGE   : "221-224"
YEAR   : "1992-00"
DOI    : "10.1007/3-540-55246-4_103"

---
MARKER : "1992_sw7_187"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Hick, P., Jackson, B.V., Schwenn, R."
TITLE  : "Synoptic maps of heliospheric Thomson scattering brightness from 1974-1985 as observed by the Helios photometers"
EDITOR : "Marsch, E., Schwenn, R."
CTITLE : "Solar Wind Seven"
SERIAL : "COSPAR Colloquia Series"
VOLUME : "3"
PAGE   : "187-190"
PUBLISH: "Pergamon, Oxford"
YEAR   : "1992"
TOPKEY : "Helios photometers"
ABS    : "We display the electron Thomson scattering intensity of the inner heliosphere as observed by the zodiacal light photometers on board the Helios spacecraft in the form of synoptic maps. The technique extrapolates the brightness information from each photometer sector near the Sun and constructs a latitude/longitude map at a given solar height. These data are unique in that they give a determination of heliospheric structures out of the ecliptic above the primary region of solar wind acceleration. The spatial extent of bright, co-rotating heliospheric structures is readily observed in the data north and south of the ecliptic plane where the Helios photometers coverage is most complete. Because the technique has been used on the complete Helios data set from 1974-1985, we observe the change in our synoptic maps with solar cycle. Bright structures are concentrated near the heliospheric equator at solar minimum, while at solar maximum bright structures are found at far higher heliographic latitudes. A comparison of these maps with other forms of synoptic data are shown for two available intervals."

---
MARKER : "1992_lnp399_322"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Webb, D.F., Altrock, R.C., Gold, R."
TITLE  : "Considerations of a Solar Mass Ejection Imager in low-earth orbit"
EDITOR : "Svestka, Z., Jackson, B.V., Machado, M.E."
CTITLE : "Eruptive Solar Flares"
SERIAL : "Lecture Notes in Physics"
VOLUME : "399"
PAGE   : "322-328"
YEAR   : "1992"
DOI    : "10.1007/3-540-55246-4_117"
TOPKEY : "Coriolis-SMEI"
ABS    : "We are designing an imager capable of observing the Thomson scattering signal from transient, diffuse features in the heliosphere [1]. The imager is expected to trace these features, which include coronal mass ejections, co-rotating structures and shock waves, to elongations greater than 90&deg; from the Sun from a spacecraft in an ~800 km Earth orbit. The predecessor of this instrument was the zodiacal-light photometer experiment on the HELIOS spacecraft which demonstrated the capability of remotely imaging transient heliospheric structures [2]. The HELIOS photometers have shown it possible to image mass ejections, co-rotating structures and the density enhancements behind shock waves. The second-generation imager we are designing, would have far higher spatial resolution enabling us to make a more complete description of these features from the Sun to 1 AU. In addition, an imager at Earth could allow up to three days warning of the arrival of a solar mass ejection."

---
MARKER : "1991_solar_phys_135_419"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "A giant coronal arch observed by Skylab"
SERIAL : "Solar Phys."
VOLUME : "135 (2)"
PAGE   : "419-422"
YEAR   : "1991-10"
DOI    : "10.1007/BF00147512"

---
MARKER : "1991_solar_phys_134_411"
TYPE   : "in_journal"
AUTHOR : "Švestka, Z."
TITLE  : "Book reviews"
SERIAL : "Solar Phys."
VOLUME : "134 (2)"
PAGE   : "411"
YEAR   : "1991-08"
DOI    : "10.1007/BF00152658"
REMARK : "book review"

---
MARKER : "1991_solar_phys_134_145"
TYPE   : "in_journal"
AUTHOR : "Fontenla, J.M., Svestka, Z., Farnik, F., Tang, F.Y."
TITLE  : "Flaring arches, III: The subflare of June 27, 1980, and its related extended arch"
SERIAL : "Solar Phys."
VOLUME : "134 (1)"
PAGE   : "145-169"
YEAR   : "1991-07"
DOI    : "10.1007/BF00148745"

---
MARKER : "1991_solar_phys_133_403"
TYPE   : "in_journal"
AUTHOR : "Hudson, H.S., Kleczek, J., Svestka, Z."
TITLE  : "Book reviews"
SERIAL : "Solar Phys."
VOLUME : "133 (2)"
PAGE   : "403-406"
YEAR   : "1991-06"
DOI    : "10.1007/BF00149899"
REMARK : "book review"

---
MARKER : "1991_lnp_387_165"
TYPE   : "in_proceedings"
TITLE  : "Evolution of hot plasma in flares"
AUTHOR : "Svestka, Z."
CTITLE : "Flare Physics in Solar Activity Maximum 22, Proc. Int. SOLAR-A Science Meeting, Tokyo, Japan, 23–26 October 1990"
EDITOR : "Uchida, Y., Canfield, R.C., Watanabe, T., Hiei, E."
SERIAL : "Lecture Notes in Physics"
VOLUME : "387"
PAGE   : "165-178"
YEAR   : "1991-05"
DOI    : "10.1007/BFb0032634"

---
MARKER : "1991_aa_244_242"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Hick, P., Jackson, B.V., Schwenn, R."
TITLE  : "Synoptic maps for the heliospheric Thomson scattering brightness as observed by the Helios photometers"
SERIAL : "Astron. Astrophys."
VOLUME : "244 (1)"
PAGE   : "242-250"
YEAR   : "1991-04"
TOPKEY : "Helios photometers"
ABS    : "We present a method for displaying the electron Thomson scattering intensity in the inner heliosphere as observed by the zodiacal light photometers on board the Helios spacecraft in the form of synoptic maps. The method is based on the assumption that the bulk of the scattering electrons along the line of sight is located near the point closest to the Sun. Inner-heliospheric structures will generally be represented properly in these synoptic maps only if they are sufficiently long-lived (that is, a significant fraction of a solar rotation period). The exmaples of Helios synoptic maps discussed (from data in April 1976 and November 1978), indicate that it is possible to identify large-scale, long-lived density enhancements in the inner heliosphere. We expect the Helios synoptic maps to be particularly useful in the study of corotating structures (e.g. streamers).  It is expected that the maps will be most reliable during periods when few transient features are present in the corona, i.e. during solar minimum."

---
MARKER : "1991_asr_11_61"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Hick, P., Jackson, B.V., Schwenn, R."
TITLE  : "Synoptic maps constructed from brightness observations of Thomson scattering by heliospheric electrons"
EDITOR : "Antonucci, E., Somov, B.V."
CTITLE : "Solar corona and solar wind"
SERIAL : "Adv. Space Res."
VOLUME : "11 (1)"
PAGE   : "61-64"
YEAR   : "1991"
DOI    : "10.1016/0273-1177(91)90091-W"
TOPKEY : "Helios photometers"
ABS    : "Observations of the Thomson scattering brightness by electrons in the inner heliosphere provide a means of probing the heliospheric electron distribution. An extensive data base of Thomson scattering observations, stretching over many years, is available from the zodiacal light photometers on board the two Helios spacecraft. A survey of these data is in progress, presenting these scattering intensities in the form of synoptic maps for successive Carrington rotations. The Thomson scattering maps reflect conditions at typically several tenths of an astronomical unit from the Sun. We discuss some representative examples from the survey in comparison with other solar/heliospheric data, such as in situ observations from the Helios plasma experiment and synoptic maps constructed from magnetic field, H&alpha; and K-coronameter data.  The comparison will provide some information about the extension of solar surface features into the inner heliosphere."

---
MARKER : "1991_asr_11_377"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Gold, R., Altrock, R."
TITLE  : "The Solar Mass Ejection Imager"
EDITOR : "Antonucci, E., Somov, B.V."
CTITLE : "Solar Corona and Solar Wind"
SERIAL : "Adv. Space. Res."
VOLUME : "11 (1)"
PAGE   : "377-381"
YEAR   : "1991"
DOI    : "10.1016/0273-1177(91)90134-6"
TOPKEY : "Coriolis-SMEI"
ABS    : "We have designed an imager capable of observing the Thomson scattering signal from transient, diffuse features in the heliosphere from a spacecraft situated near 1 AU. The imager is expected to trace these features, which include coronal mass ejections, co-rotating structures and shock waves, to elongations greater than 90&deg; from the Sun. The instrumentation ultimately may be regarded as a successor to the heliospheric imaging cabability shown possible by the zodiacal-light photometers of the HELIOS spacecraft. The second-generation instrument we have designed, would make far more effective use of View the MathML source solar wind data from spacecraft in the vicinity of the imager by extending these observations to the structures surrounding it. In addition, an imager at Earth could allow up to three days warning of the arrival of a mass ejection from the Sun."

---
MARKER : "1991_adv_space_res_11_115"
TYPE   : "in_proceedings"
TITLE  : "Needs and constraints for solar flares space-borne cooperative programs"
AUTHOR : "Svestka, Z."
SERIAL : "Adv. Space Res."
VOLUME : "11 (5)"
PAGE   : "115-121"
YEAR   : "1991-00"
DOI    : "10.1016/0273-1177(91)90367-S"

---
MARKER : "1991_yohkoh_mission_invited"
TYPE   : "proceedings"
EDITOR : "Svestka, Z., Uchida, Y."
TITLE  : "The Yohkoh (Solar-A) mission: a series of invited contributions"
YEAR   : "1991-00"
PUBLISH: "Kluwer Academic Publ."

---
MARKER : "1990_solar_phys_129_363"
TYPE   : "in_journal"
AUTHOR : "Poletto, G., Svestka, Z."
TITLE  : "Real-time simulation of a potential magnetic field in a post-flare arch"
SERIAL : "Solar Phys."
VOLUME : "129 (2)"
PAGE   : "363-377"
YEAR   : "1990-10"
DOI    : "10.1007/BF00159047"

---
MARKER : "1990_aa_233_252"
TYPE   : "in_journal"
AUTHOR : "Standish, E.M."
TITLE  : "The observational basis for JPL's DE 200, the planetary ephemerides of the Astronomical Almanac"
SERIAL : "Astron. Astrophysics"
VOLUME : "233 (1)"
PAGE   : "252-271"
YEAR   : "1990-07"
TOPKEY : "ephemeris"
ABS    : "The Jet Propulsion Laboratory's ephemerides, DE200/LE200, now form the basis for the planetary and lunar positions listed in most of the major national almanacs throughout the world. They have resulted from a least squares' adjustment to a wide variety of observational data totaling over 50000 positional measurements. These data types include optical data (transit and photographic), radar-ranging, spacecraft ranging and laser-ranging. This paper documents the planetary observational data used in the series of ephemerides produced at JPL over the six years preceding the cration of DE118/LE62, the set which was transformed directly into the JD2000-based set, DE200/LE200. The major planetary ephemerides in this period of evolution were DE96, DE102, DE108, DE111 and DE118. The paper also presents details of the procedures involved in the data reductions. For the optical data reductions, the paper includes corrections for planetary limb biases, phase effects, day-night differences, catalogue drifts and catalogue offsets. For the radar ranges, the basic light-time equation includes Earth orientation, station location and reflection point location; it is augmented by correcttions for the time delays due to general relativity, the electron content of the solar corona and the troposphere. Further, techniques to overcome the uncertainties due to planetary topography are described, including closure point analysis and occultation point comparisons. For the spacecraft data, the basic reductions, similar to those for radar, are augmented by formulations for locating the transponder, whether in orbit or landed on the surface of a planet. The total set of observational data contained at JPL represents a unique collection. Some of the data are published in the various astronomical journals and have been retrieved directly from these sources; some were sent personally to JPL by the observer; some of the data originated at JPL itself. Some of the data are in the possession of many astronomers throughout the world; some are kept only at various locations within JPL; some may be only in the possession of the planetary ephemeris group at JPL. The complete data set has been archived onto magnetic tape. The providers of the data are acknowledged."

---
MARKER : "1990_solar_phys_127_149"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z., Farník, F., Tang, F."
TITLE  : "X-ray bright surges"
SERIAL : "Solar Phys."
VOLUME : "127 (1)"
PAGE   : "149-163"
YEAR   : "1990-05"
DOI    : "10.1007/BF00158520"

---
MARKER : "1990_solar_phys_126_411"
TYPE   : "in_journal"
AUTHOR : "Mewe, R., Svestka, Z."
TITLE  : "Book reviews"
SERIAL : "Solar Phys."
VOLUME : "126 (2)"
PAGE   : "411"
YEAR   : "1990-04"
DOI    : "10.1007/BF00153061"
REMARK : "book review"

---
MARKER : "1989_solar_phys_124_339"
TYPE   : "in_journal"
AUTHOR : "Martin, S.F., Svestka, Z.F., Bhatnagar, A."
TITLE  : "The footpoints of giant arches"
SERIAL : "Solar Phys."
VOLUME : "124 (2)"
PAGE   : "339-352"
YEAR   : "1989-09"
DOI    : "10.1007/BF00156274"

---
MARKER : "1989_solar_phys_123_317"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z., Farník, F., Fontenla, J.M., Martin, S.F."
TITLE  : "Flaring arches, II: Events in the arch system of 6/7 November, 1980"
SERIAL : "Solar Phys."
VOLUME : "123 (2)"
PAGE   : "317-341"
YEAR   : "1989-09"
DOI    : "10.1007/BF00149109"

---
MARKER : "1989_solar_phys_119_419"
TYPE   : "in_journal"
AUTHOR : "Poletto, G., Dimitrov, D.L., Svestka, Z."
TITLE  : "Book reviews"
SERIAL : "Solar Phys."
VOLUME : "119 (2)"
PAGE   : "419-420"
YEAR   : "1989-09"
DOI    : "10.1007/BF00146189"
REMARK : "book review"

---
MARKER : "1989_solar_phys_122_111"
TYPE   : "in_journal"
AUTHOR : "Hick, P., Priest, E.R."
TITLE  : "Slow-shock Heating in post-flare arches"
SERIAL : "Solar Phys."
VOLUME : "122 (1)"
PAGE   : "111-129"
YEAR   : "1989-03"
DOI    : "10.1007/BF00162830"
TOPKEY : "post-flare arch, flares"
ABS    : "The heating of a coronal arch following the occurrence of a dynamic (two-ribbon) flare is discussed, investigating whether slow-shock heating, occurring during the reconnection process in the dynamic flare and responsible for the heating of the post-flare loops, is also a workable proposition for the heating of a coronal arch. Contrary to the flare loops, the shock structure in the arch is generally not modified greatly by thermal conduction effects. As a result slow-shock heating may be investigated in terms of the familiar MHD-shock jump relations. The observed enhanced arch density with respect to the surrounding corona is explained as a direct consequence of the reconnection process. For a combination of high arch temperatures and low values of coronal magnetic field and density thermal conduction may become important and will lead to an extra density enhancement in the arch. An interpretation of the arch of May 21-22, 1980 suggests that the formation of the arch took approximately 1 hour, and that observed temperature, density, and maximum energy content can be consistently explained by the slow-shock heating mechanism."

---
MARKER : "1989_solar_phys_122_131"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z.F., Jackson, B.V., Howard, R.A., Sheeley, N.R."
TITLE  : "Giant solar arches and coronal mass ejections in November 1980"
SERIAL : "Solar Phys."
VOLUME : "122 (1)"
PAGE   : "131-143"
YEAR   : "1989-03"
DOI    : "10.1007/BF00162831 "

---
MARKER : "1989_solar_phys_122_191"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Book reviews"
SERIAL : "Solar Phys."
VOLUME : "122 (1)"
PAGE   : "191-192"
YEAR   : "1989-03"
DOI    : "10.1007/BF00162835"
REMARK : "book review"

---
MARKER : "1989_solar_phys_121_ix"
TYPE   : "in_journal"
AUTHOR : "de Jager, C., Švestka, Z., Howard, R.F."
TITLE  : "Editorial topical issue 'Solar and stellar flares'"
SERIAL : "Solar Phys."
VOLUME : "121 (1-2)"
PAGE   : "ix"
YEAR   : "1989-03"
DOI    : "10.1007/BF00161682"
REMARK : "book review"

---
MARKER : "1989_solar_phys_121_399"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Solar flares: The gradual phase"
CTITLE : "Proc. Coll. on Solar and stellar flares"
PLACE  : "Stanford, CA, US, 15-19 August 1988"
SERIAL : "Solar Phys."
VOLUME : "121 (1-2)"
PAGE   : "399-417"
YEAR   : "1989-03"
DOI    : "10.1007/BF00161709"

---
MARKER : "1989_aa_210_399"
TYPE   : "in_journal"
AUTHOR : "Leinert, C., Pitz, E."
TITLE  : "Zodiacal light observed by Helios throughout Solar Cycle No. 21: stable dust and varying plasma"
SERIAL : "Astron. Astrophys."
VOLUME : "210"
PAGE   : "399-402"
YEAR   : "1989-02"
TOPKEY : "ephemeris"
ABS    : "The zodiacal light observations performed by the Helios space probes covered a period of more than 11 years, from December 1974 through February 1986. During this time no variation in zodiacal light brightness was detected, with limits of + or - 2 percent for secular variations. However, the density of solar wind at high heliographic latitudes showed a strong enhancement during the maximum of solar cycle."

---
MARKER : "1989_geophys_mono_54_291"
TYPE   : "in_proceedings"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V., Hudson, H.S., Nichols, J.D., Gold, R.E."
TITLE  : "Design considerations for a 'Solar Mass Ejection Imager' on a rotating spacecraft"
EDITOR : "Waite Jr., J.H., Burch, J.L., Moore, R.L."
CTITLE : "Solar System Plasma Physics"
SERIAL : "Geophysical Monograph"
VOLUME : "54"
PAGE   : "291-297"
YEAR   : "1989"
DOI    : "10.1029/GM054p0291"
TOPKEY : "Coriolis-SMEI"
ABS    : "We describe an instrument capable of imaging the time-varying features of the entire outer corona (from near the Sun to beyond 90&deg; elongation) via the Thomson-scattered diffuse solar light. This 'all sky' imager works on a spin-stabilized spacecraft, preferably in deep space. The design for such an imager, which can for example study solar mass ejections at great distances from the Sun, must deal with spurious signals from stray light, zodiacal light, and stars to surface brightness levels below 1 S10 unit. The design discussed here envisions a set of three slit apertures, feeding one-dimensional detectors through a lens system; the spacecraft rotation allows a complete sky survey during each spin of the spacecraft. Data clocked into a computer memory complete the 'image' of the whole sky. We have analyzed a 'median filter' approach to reducing the effects of starlight, in real time, on the statistics of the residual diffuse background. The analysis also included simulations of spacecraft nutation, spin-phase timing error, and image quality in the necessary wide-field optics."

---
MARKER : "1989_assl_153_493"
TYPE   : "in_proceedings"
AUTHOR : "Hildner, E., Bassi, J., Bougeret, J.L., Duncan, R.A., Gary, D.E., Gergely, T.E., Harrison, R.A., Howard, R.A., Illing, R.M.E., Jackson, B.V., Kahler, S.W., Kopp, K., Low, B.C., Lantos, P., Phillips, K.J.H., Poletto, G., Sheeley, N.R. Jr., Steward, R.T., Svestka, Z., Waggett, P.W., Wu, S.T."
TITLE  : "Coronal mass ejections and coronal structures"
SERIAL : "Astrophysics and Space Science Library"
VOLUME : "153"
EDITOR : "Kundu, M.R., Woodgate, E., Schmahl, E.J."
CTITLE : "Proc. Energetic phenomena on the Sun"
PAGE   : "493-596"
YEAR   : "1989-00"
DOI    : "10.1007/978-94-009-2331-7_6"
PLACE  : "Goddard Space Flight Center, Greenbelt, MD, US (1983-01-24/28, 1983-06-08/14, 1984-02-13/17)"
ABS    : "The coronal portion of the solar atmosphere consists of a wide variety of structures which exhibit a similarly wide variety of dynamical processes and kinds of activity. The launch of the SMM presented an opportunity to study the low and intermediate corona from space with multiple instruments for protracted periods of time. This opportunity had been lacking for years, and it was enthusiastically awaited by those interested in coronal studies. The research performed during the SMM Workshop and reported here shows how successfully the SMM and collaborative observations have been used to advance our knowledge of the corona and how these observations have stimulated our theoretical understanding of why the corona is the way we observe it to be."

---
MARKER : "1988_solar_phys_116_91"
TYPE   : "in_journal"
AUTHOR : "Martin, S.F., Svestka, Z."
TITLE  : "Flaring arches, I. The major events of 1980 November 6 and 12"
SERIAL : "Solar Phys."
VOLUME : "116 (1)"
PAGE   : "91-118"
YEAR   : "1988-09"
DOI    : "10.1007/BF00171717"

---
MARKER : "1988_solar_phys_115_327"
TYPE   : "in_journal"
AUTHOR : "Jackson, B.V., Rompolt, B., Svestka, Z."
TITLE  : "Solar and interplanetary observations of the mass ejection on 7 May, 1979"
SERIAL : "Solar Phys."
VOLUME : "115 (2)"
PAGE   : "327-343"
YEAR   : "1988-09"
DOI    : "10.1007/BF00148732 "

---
MARKER : "1988_solar_phys_115_409"
TYPE   : "in_journal"
AUTHOR : "Kleczek, J., Svestka, Z."
TITLE  : "Book reviews"
SERIAL : "Solar Phys."
VOLUME : "115 (2)"
PAGE   : "409"
YEAR   : "1988-09"
DOI    : "10.1007/BF00148737"
REMARK : "book review"

---
MARKER : "1988_afgl_tr_88_0195"
TYPE   : "tech. report"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V."
TITLE  : "Scientific background and design specifications for a near-Earth heliospheric imager"
PUBLISH: "Air Force Geophysics Laboratory"
VOLUME : "AFGL-TR-88-0195"
YEAR   : "1988-08"
TOPKEY : "Coriolis-SMEI"
ABS    : "This report is intended to define the instrument specifications for a heliospheric imager capable of observing transient, diffuse features in the heliosphere from a spacecraft near 1 AU. These features include coronal mass ejections, co-rotating density enhancements, shock waves and any other disturbances that can affect the intensity of the electron-scattering coronal brightness. Our technique of imaging a large portion of the heliosphere using the HELIOS spacecraft zodiacal-light photometers has shown that it is possible to measure the structures around a spacecraft and to make good measurements of material in and out of the ecliptic plane. The HELIOS data show that is is posible to determine the velocityes and spatial distributions of the large-scale features which propagate into the heliosphere. The instrumentation may be regarded as a successor to the zodiacal-light photometers of the HELIOS spacecraft. Such a second-generation instrument based on these principals could make effective use of in situ solar wind data from spacecraft in the vicinity of the imager, and would allow study of the effects of heliospheric structure interaction with the magnetosphere as never before possible. In addition, the imager would allow up to three days warning of the arrival of a mass ejection at Earth from the Sun."

---
MARKER : "1988_thesis_phick"
TYPE   : "PhD thesis"
AUTHOR : "Hick, P."
TITLE  : "Interpretations of energetic phenomena in the solar corona"
PUBLISH: "University of Utrecht, Netherlands"
YEAR   : "1988-04"
TOPKEY : "X-rays, cosmic rays"

---
MARKER : "1988_solar_phys_115_203"
TYPE   : "in_journal"
AUTHOR : "Kotov, V.A., Kostik, R., Shchukina, N., Svestka, Z."
TITLE  : "Book reviews"
SERIAL : "Solar Phys."
VOLUME : "115 (1)"
PAGE   : "203-204"
YEAR   : "1988-03"
DOI    : "10.1007/BF00146240"
REMARK : "book review"

---
MARKER : "1988_adv_space_res_8_81"
TYPE   : "in_proceedings"
TITLE  : "Soft X-ray observations of large-scale coronal structures"
AUTHOR : "Svestka, Z."
SERIAL : "Adv. Space Res."
VOLUME : "8 (11)"
PAGE   : "81-86"
YEAR   : "1988-00"
DOI    : "10.1016/0273-1177(88)90299-2"

---
MARKER : "1987_solar_phys_114_389"
TYPE   : "in_journal"
AUTHOR : "Gaizauskas, V., Svestka, Z."
TITLE  : "Highlights of the flare build-up study"
SERIAL : "Solar Phys."
VOLUME : "114 (2)"
PAGE   : "389-398"
YEAR   : "1987-09"
DOI    : "10.1007/BF00167354"

---
MARKER : "1987_solar_phys_114_329"
TYPE   : "in_journal"
AUTHOR : "Hick, P., Svestka, Z., Smith, K.L., Strong, K.T."
TITLE  : "Post-flare coronal arches observed with the SMM/XRP Flat Crystal Spectrometer"
SERIAL : "Solar Phys."
VOLUME : "114 (2)"
PAGE   : "329-345"
YEAR   : "1987-09"
DOI    : "10.1007/BF00167349"
TOPKEY : "post-flare arch, flares"
ABS    : "The phenomenon of post-flare coronal arches, initially discovered with the Hard X-Ray Imaging Spectrometer (HXIS), was investigated using observations made with the SMM Flat Crystal Spectrometer on 20 through 23 January, 1985. Since these observations were made with a different type of instrument from HXIS, they provide independent information on the physical characteristics of the arch phenomenon and extend our knowledge to lower coronal temperatures."

---
MARKER : "1987_solar_phys_108_315"
TYPE   : "in_journal"
AUTHOR : "Hick, P., Svestka, Z."
TITLE  : "Thermal structures associated with post-flare coronal arches"
SERIAL : "Solar Phys."
VOLUME : "108 (2)"
PAGE   : "315-331"
YEAR   : "1987-09"
DOI    : "10.1007/BF00214167"
TOPKEY : "post-flare arch"
ABS    : "On 6-7 November, 1980, the Hard X-ray Imaging Spectrometer on board the Solar Maximum Mission observed a sequence of extensive post-flare coronal arches (Svestka et al., 1982; Svestka, 1984). Each arch was preceded by a dynamic (two-ribbon) flare. Each dynamic flare apparently initiated a renewed heating of plasma in a pre-existing coronal magnetic structure, thus creating the next arch in the sequence; hence, the term 'arch revival' (Svestka, 1984). From observations of the post-flare corona after all three parent flares in the coarse field of view Svestka (1984) deduced a velocity pattern in each of the revived arches consisting of two components. A fast component and a slow component. The authors discuss the slow component of the velocity pattern, (in particular the associated thermal structures) as observed after the dynamic flares giving rise to the 6-7 November arches and the dynamic flare on 4 June, 1980, 07:53 UT. Furthermore, the observation that no disturbance was present after the occurrence of a confined flare, starting on 17:25 UT of 6 November, 1980, is of importance for the interpretation of these thermal structures.  The effects of conduction and radiative cooling and their consequences for the disturbed region are discussed. A qualitative scenario for the revival of a coronal arch, incorporating the phenomenon of the moving disturbance, is presented, and the authors discuss the relation of the disturbance to the reconnection region."

---
MARKER : "1987_solar_phys_108_411"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Cooling of a coronal flare loop through radiation and conduction"
SERIAL : "Solar Phys."
VOLUME : "108 (2)"
PAGE   : "411-414"
YEAR   : "1987-09"
DOI    : "10.1007/BF00214172"

---
MARKER : "1987_solar_phys_108_237"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z.F., Fontenla, J.M., Machado, M.E., Martin, S.F., Neidig, D.F., Poletto, G."
TITLE  : "Multi-thermal observations of newly formed loops in a dynamic flare"
SERIAL : "Solar Phys."
VOLUME : "108 (2)"
PAGE   : "237-250"
YEAR   : "1987-09"
DOI    : "10.1007/BF00214164"

---
MARKER : "1987_aa_172_350"
TYPE   : "in_journal"
AUTHOR : "Hick, P., Stevens, G."
TITLE  : "Approximate solutions to the cosmic ray transport equation: the maximum entropy method"
SERIAL : "Astron. Astrophys."
VOLUME : "172 (1-2)"
PAGE   : "350-358"
YEAR   : "1987-01"
TOPKEY : "cosmic rays"
ABS    : "We describe a method to obtain approximate solutions to a differential equation involving a density function in accordance with Jaynes (1957) principle of maximum entropy. The method uses some known moments of the real solution, obtained directly from the differential equation. Jaynes' principle provides a criterion necessary to construct from these moments an approximation to the real solution. After some introductory examples the authors apply the maximum entropy method to simple forms of the cosmic ray transport equation. They compare the resulting approximation, as well as the familiar diffusion approximation, with a numerical solution. They find that there is qualitative agreement between the maximum entropy approximation and the numerical solution, and that their method is a significant improvement on the diffusion approximation, especially in its description of the first order anisotropy."

---
MARKER : "1987_solar_phys_113_67"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Relationships among flare images at different wavelengths"
SERIAL : "Solar Phys."
VOLUME : "113 (1-2)"
PAGE   : "67-86"
YEAR   : "1987-00"
DOI    : "10.1007/BF00147684"

---
MARKER : "1987_solar_phys_113_303"
TYPE   : "in_journal"
AUTHOR : "Martin, S.F., Svestka, Z."
TITLE  : "Flaring arches"
SERIAL : "Solar Phys."
VOLUME : "113 (1-2)"
PAGE   : "303-304"
YEAR   : "1987-00"
DOI    : "10.1007/BF00147713"

---
MARKER : "1987_sw6_272"
TYPE   : "in_proceedings"
AUTHOR : "Jackson, B.V., Rompolt, B., Svestka, Z."
TITLE  : "Solar and interplanetary observations of the mass ejection on 7 May 1979"
EDITOR : "Pizzo, V.J., Holzer, T., Sime, D.G."
CTITLE : "Proc. on Solar Wind 6"
PLACE  : "Estes Park, CO, US, 23-28 August 1987"
VOLUME : "2"
PAGE   : "272"
YEAR   : "1987-00"
PUBLISH: "NCAR"

---
MARKER : "1986_nasa_cp_2439_chapt_6"
TYPE   : "in_proceedings"
AUTHOR : "Hildner, E., Bassi, J., Bougeret, J.L., Duncan, R.A., Gary, D.E., Gergely, T.E., Harrison, R.A., Howard, R.A., Illing, R.M.E., Jackson, B.V., Kahler, S.W., Kopp, K., Low, B.C., Lantos, P., Phillips, K.J.H., Poletto, G., Sheeley, N.R. Jr., Steward, R.T., Svestka, Z., Waggett, P.W., Wu, S.T."
TITLE  : "Coronal mass ejections and coronal structures"
EDITOR : "Kundu, M., Woodgate, B."
SERIAL : "NASA-CP"
VOLUME : "2439"
CHAPTER: "6"
CTITLE : "Energetic phenomena on the Sun: the Solar Maximum Mission Flare Workshop Proc."
PAGE   : "(71 pages)"
YEAR   : "1986-12"
URL    : "http://ntrs.nasa.gov/search.jsp?R=19870009895&hterms=Energetic+Phenomena+Sun&qs=N%3D0%26Ntk%3DAll%26Ntx%3Dmode%2Bmatchallany%26Ntt%3DEnergetic%2BPhenomena%2Bon%2Bthe%2BSun"
REMARK : "Also published as ASSL, Vol. 153, in 1989"

---
MARKER : "1986_research_tool_41"
TYPE   : "in_book"
AUTHOR : "Svestka, Z."
TITLE  : "X-ray imaging of flare loops and coronal arches"
CTITLE : "Solar flares and coronal physics using P/OF as a research tool"
SERIAL : "NASA Conf. Publ."
VOLUME : "2421"
PAGE   : "41-66"
YEAR   : "1986-04"
PUBLISH: "NASA"

---
MARKER : "1987_solar_phys_114_193"
TYPE   : "in_journal"
AUTHOR : "Schindler, K., Svestka, Z."
TITLE  : "Book reviews"
SERIAL : "Solar Phys."
VOLUME : "114 (1)"
PAGE   : "193"
YEAR   : "1987-03"
DOI    : "10.1007/BF00193080"
REMARK : "book review"

---
MARKER : "1986_solar_phys_107_200"
TYPE   : "in_journal"
AUTHOR : "de Jager, C., Svestka, Z."
TITLE  : "Editorial"
SERIAL : "Solar Phys."
VOLUME : "107 (1)"
PAGE   : "200"
YEAR   : "1986-03"
DOI    : "10.1007/BF00155354"
REMARK : "editorial"

---
MARKER : "1987_solar_phys_108_201"
TYPE   : "in_journal"
AUTHOR : "Hick, P., Jackson, B., Svestka, Z., Krivsky, L."
TITLE  : "Book reviews"
SERIAL : "Solar Phys."
VOLUME : "108 (1)"
PAGE   : "201-203"
YEAR   : "1987-03"
DOI    : "10.1007/BF00152089"
REMARK : "book review"

---
MARKER : "1986_asr_06_271"
TYPE   : "in_proceedings"
AUTHOR : "Hick, P."
TITLE  : "An interruption of the cooling of the coronal arch of 6/7 November 1980"
EDITOR : "Svestka, Z., de Jager, C."
CTITLE : "The Solar Maximum Year"
SERIAL : "Adv. Space Res."
VOLUME : "6 (6)"
PAGE   : "271-274"
YEAR   : "1986-00"
DOI    : "10.1016/0273-1177(86)90158-4"
TOPKEY : "post-flare arch, flares"
ABS    : "During the decay phase of the giant coronal arch, which appeared after the dynamic flare of 14:44 UT on 6 November 1980, the cooling of the arch was interrupted for a period of two hours from 18 UT until 20 UT. In the upper parts of the arch (above 12 &times; 10^4 km) the temperature rose again. At lower altitudes the decline in temperature was only slowed down. The energy input was an increasing function of altitude and for the whole arch amounted to 7&times;10^29 erg. A thermal disturbance, formed after the dynamic flare low in the corona and subsequently rising upward, moves through the old arch in the same period. The reconnection which accompanies the coalescence of the magnetic field structures of the disturbance and the old arch is probably responsible for the energy release."

---
MARKER : "1986_solar_phys_104_321"
TYPE   : "in_journal"
AUTHOR : "Farnik, F., van Beek, H.F., Svestka, Z."
TITLE  : "Coronal interconnection of two active regions observed in 3.5–8.0 keV X-rays"
SERIAL : "Solar Phys."
VOLUME : "104 (2)"
PAGE   : "321-332"
YEAR   : "1986-04"
DOI    : "10.1007/BF00159085"

---
MARKER : "1986_solar_phys_104_187"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z., Hick, P."
TITLE  : "Images of post-flare coronal structures in X-rays"
SERIAL : "Solar Phys."
VOLUME : "104 (1)"
PAGE   : "187-190"
YEAR   : "1986-03"
DOI    : "10.1007/BF00159961"

---
MARKER : "1986_solar_phys_104_187"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z., Hick, P."
TITLE  : "Images of post-flare coronal structures in X-rays"
SERIAL : "Solar Phys."
VOLUME : "104 (1)"
PAGE   : "187-190"
EDITOR : "Benz, A.O."
CTITLE : "Radio continua during solar flares"
PUBLISH: "D. Reidel Publ. Co., Dordrecht, Netherlands"
YEAR   : "1986-03"
DOI    : "10.1007/BF00159961"
TOPKEY : "post-flare arch, flares"
ABS    : "Extensive coronal structures related to radio continua and imaged in X-rays of more than 3.5 keV are described. Data obtained by the Hard X-ray Imaging Spectrometer aboard the SMM satellite reveal that variations in X-ray and radio emission take place inside an arch-encircling plasmoid. These variations are caused by a process whereby particles accelerated in the upper part of the plasmoid stream down the magnetic field lines and in effect heat the lower part of the plasmoid. It is noted that this process can explain why particles streaming along the field lines avoid the arch top so that the arch itself is not affected and why variations start only after the plasmoid is formed (several hours after the flare)."

---
MARKER : "1986_solar_phys_103_399"
TYPE   : "in_journal"
AUTHOR : "McCabe, M.K., Svestka, Z.F., Howard, R.A., Jackson, B.V., Sheeley, N.R."
TITLE  : "Coronal mass ejection associated with the stationary post-flare arch of 21–22 May 1980"
SERIAL : "Solar Phys."
VOLUME : "103 (2)"
PAGE   : "399-408"
YEAR   : "1986-02"
DOI    : "10.1007/BF00147838"

---
MARKER : "1986_lower_atmosphere_of_solar_flares_489"
TYPE   : "in_proceedings"
AUTHOR : "Canfield, R.C., Gaizauskas, V., Kurokawa, H., Martin, S.F., Svestka, Z."
TITLE  : "Observations of chromospheric flare dynamics at the next solar maximum specific recommendations of the Chromospheric Flare Dynamics Group"
EDITOR : "Neidig, D.F."
CTITLE : "Proc. Solar Maximum Mission Symp. on The lower atmosphere of solar flares, relationships between low temperature plasmas and high energy emissions"
PLACE  : "Sunspot, NM, US, 20-24 August 1985"
PAGE   : "489-490"
YEAR   : "1986-02"
PUBLISH: "NSO/SacPeak Publ."

---
MARKER : "1986_lower_atmosphere_of_solar_flares_483"
TYPE   : "in_proceedings"
AUTHOR : "Machado, M.E., Avrett, E.H., Falciani, R., Fang, C., Gesztelyi, L., Henoux, J.-C., Hiei, E., Neidig, D.F., Rust, D.M., Sotirovski, P., Svestka, Z., Zirin, H."
TITLE  : "White light flares and atmospheric modeling (Working Group report)"
EDITOR : "Neidig, D.F."
CTITLE : "Proc. Solar Maximum Mission Symp. on The lower atmosphere of solar flares, relationships between low temperature plasmas and high energy emissions"
PLACE  : "Sunspot, NM, US, 20-24 August 1985"
PAGE   : "483"
YEAR   : "1986-02"
PUBLISH: "NSO/SacPeak Publ."

---
MARKER : "1986_lower_atmosphere_of_solar_flares_332"
TYPE   : "in_proceedings"
AUTHOR : "Svestka, Z."
TITLE  : "On the varieties of solar flares"
EDITOR : "Neidig, D.F."
CTITLE : "Proc. Solar Maximum Mission Symp. on The lower atmosphere of solar flares, relationships between low temperature plasmas and high energy emissions"
PLACE  : "Sunspot, NM, US, 20-24 August 1985"
PAGE   : "332-355"
YEAR   : "1986-02"
PUBLISH: "NSO/SacPeak Publ."

---
MARKER : "1986_adv_space_res_6_253"
TYPE   : "in_proceedings"
TITLE  : "A dynamic flare with anomalously dense flare loops"
AUTHOR : "Svestka, Z., Fontenla, J.M., Machado, M.E., Martin, S.F., Neidig, D.F., Poletto, G."
SERIAL : "Adv. Space Res."
VOLUME : "6 (6)"
PAGE   : "253-256"
YEAR   : "1986-00"
DOI    : "10.1016/0273-1177(86)90155-9"

---
MARKER : "1986_adv_space_res_6_5"
TYPE   : "in_proceedings"
TITLE  : "Flare build-up study summary"
AUTHOR : "Gaizauskas, V., Svestka, Z."
SERIAL : "Adv. Space Res."
VOLUME : "6 (6)"
PAGE   : "5-6"
YEAR   : "1986-00"
DOI    : "10.1016/0273-1177(86)90104-3"

---
MARKER : "1986_adv_space_res_6"
TYPE   : "proceedings"
EDITOR : "de Jager, C., Svestka, Z."
TITLE  : "The physics of solar flares"
PLACE  : "COSPAR 26, Toulouse, France, 30 June-11 July 1986"
SERIAL : "Adv. Space Res."
VOLUME : "6 (6)"
PAGE   : "(365 pages)"
YEAR   : "1986"

---
MARKER : "1986_solar_physic_centennial"
TYPE   : "book"
EDITOR : "de Jager, C., Svestka, Z."
TITLE  : "Progress in solar physics : review papers invited to celebrate the centennial volume of Solar physics"
YEAR   : "1986-00"
PUBLISH: "Reidel, Dordrecht"

---
MARKER : "1986_eslab_19_355"
TYPE   : "in_proceedings"
AUTHOR : "Hick, P., Stevens, G., van Rooijen, J."
TITLE  : "The maximum entropy principle in cosmic ray transport theory"
CTITLE : "19^th ESLAB symposium: The Sun and the heliosphere in three dimensions"
SERIAL : "Astrophysics and Space Science Library"
VOLUME : "123"
PAGE   : "355-358"
PUBLISH: "D. Reidel Publ. Co., Dordrecht, Netherlands"
YEAR   : "1986-00"
PLACE  : "Les Diablerets, CH, 4-6 June 1985"
TOPKEY : "cosmic rays"
ABS    : "A procedure to obtain an approximate solution to the cosmic ray transport equation, which, contrary to the familiar diffusion approximation, is valid also for large anisotropies is described. Using some moments of the distribution function an approximation is constructed, in accordance with Jaynes (1957) principle of maximum entropy. The procedure is applied to the case of the one-dimensional transport equation and the resulting Maximum Entropy approximation and the diffusion approximation with the numerical solution are compared, that there is a qualitative agreement between the maximum entropy approximation and the numerical solution, particularly close to the particle source where the diffusion approximation breaks down."

---
MARKER : "1986_asr_06_307"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B."
TITLE  : "HELIOS photometer measurements of in-situ density enhancements"
SERIAL : "Adv. Space Res."
VOLUME : "6 (6)"
PAGE   : "307-310"
YEAR   : "1986-00"
DOI    : "10.1016/0273-1177(86)90165-1"
PUBLISH: "Elsevier"
TOPKEY : "Helios photometers"
ABS    : "The HELIOS spacecraft zodiacal light photometers have been used to image coronal mass ejections and coronal streamers in the interplanetary medium. The HELIOS photometers have the ability to image such features beyond 90&deg; angular distance from the Sun. This provides a unique opportunity to measure brightness enhancements which are also observed as density increases in situ by the HELIOS spacecraft plasma probes. Here, I compare the brightness enhancements and in situ density increases following shocks defined by the plasma and magnetic field data. Five well-observed shocks from 1976 and 1979 illustrate these comparisons. Each event can be followed in photometer data as it sweeps past the HELIOS spacecraft. To first order, the enhancements of brightness following shocks indicate structures which extend over many tenths of an astronomical unit and colors which are consistent with Thomson scattering of sunlight by electrons."

---
MARKER : "1985_solar_phys_102_147"
TYPE   : "in_journal"
AUTHOR : "Hick, P., Svestka, Z."
TITLE  : "The stationary post-flare arch of May 21/22, 1980"
SERIAL : "Solar Phys."
VOLUME : "102 (1-2)"
PAGE   : "147-158"
YEAR   : "1985-12"
DOI    : "10.1007/BF00154044"

---
MARKER : "1985_solar_phys_102_147"
TYPE   : "in_journal"
AUTHOR : "Hick, P., Svestka, Z."
TITLE  : "The stationary post-flare arch of May 21/22 1980"
SERIAL : "Solar Phys."
VOLUME : "102 (1/2)"
PAGE   : "147-158"
YEAR   : "1985-12"
DOI    : "10.1007/BF00154044"
TOPKEY : "post-flare arch, flares"
ABS    : "On May 21/22, 1980 the Hard X-Ray Imaging Spectrometer aboard the SMM imaged an extensive coronal structure after the occurrence of a two-ribbon flare on May 21, 20:50 UT. The structure was observed from 22:20 UT on May 21 until its disappearence at 09:00 UT on May 22.  

At 22:20 UT the brightest pixel in the arch was located at a projected altitude of 95 000 km above the zero line of the longitudinal magnetic field. At 23:02 UT the maximum of brightness shifted to a neighbouring pixel with approximately the same projected altitude. This sudden shift indicates that the X-ray structure consisted of (at least) two separate arches at approximately the same altitude, one of which succeeded the other as the brightest arch in the structure at 23:02 UT.

From 23:02 UT onwards the maximum of brightness did not change its position in the HXIS coarse field of view. With a spatial resolution of 32 arcsec this places an upper limit of 1.1 km s^&minus;1 on the rise velocity of the arch. Thus, contrary to a similar arch observed on November 6/7, where rise velocities of the order of 10 km s-1 were measured in the same phase of development, the May 22 arch was a stationary structure at an altitude of &asymp;145000 km.

The following values were estimated for the physically relevant quantities of the May 21/22 arch at the time of its maximum brightness (&asymp;23:00 UT): temperature T&asymp;6.3&times;106 K, electron density n_e&asymp;1.1&times;109 cm^&minus;3, total emitting volume V&asymp;5&times;10^29 cm^3, energy density &epsilon;&asymp;2.9 erg cm^&minus;3, total energy contents E&asymp;1.4&times;10^30 erg, total mass M&asymp;9&times;10^14 g.

The top of the arch was observed at &asymp;145 000 km altitude within 1.5 hr after the flare occurrence. Since it seems unlikely that the structure already existed prior to the flare at 20:50 UT, the arch must have risen to its stationary position with an average velocity exceeding 17 km s^&minus;1 (possibly much faster). We speculate that the arch was formed very fast at the flare onset, when (part of) the active region loop system was elevated within minutes to the observed altitude."

---
MARKER : "1985_solar_phys_100_563"
TYPE   : "in_journal"
AFFIL  : "UCSD-CASS-SHPG"
AUTHOR : "Jackson, B.V."
TITLE  : "Imaging of coronal mass ejections by the Helios spacecraft"
SERIAL : "Solar Phys."
VOLUME : "100"
PAGE   : "563-574"
YEAR   : "1985-10"
DOI    : "10.1007/BF00158445"
TOPKEY : "coronal mass ejections, Helios photometers"
ABS    : "The zodiacal light photometers on board the HELIOS spacecraft can be used to form images of coronal mass ejections in the interplanetary medium. Several aspects of these data are unique: they trace coronal mass ejections using Thomson scattering techniques to distances from the Sun greater than 0.5 AU; their perspective from the HELIOS orbits allow information to be gained about the three-dimensional shapes of specific mass ejections viewed both by coronagraphs and HELIOS; the global view afforded by the spacecrafts photometers can image the mass ejection from within and thus relate in situ measurements to the shape of the whole structure. To date, the HELIOS photometers have been used to study coronagraph-observed mass ejections including those which originate at the Sun on 7 May, 24 May, and 27 November, 1979, and 21 May, 18 June, 29 June, and 6 November, 1980. Masses of ejections determined from these data are generally a few times larger than masses determined from SOLWIND coronagraph images."

---
MARKER : "1985_solar_phys_100_435"
TYPE   : "in_journal"
AUTHOR : "de Jager, C., Svestka, Z."
TITLE  : "21 May 1980 flare review"
SERIAL : "Solar Phys."
VOLUME : "100 (1-2)"
PAGE   : "435-463"
YEAR   : "1985-10"
DOI    : "10.1007/BF00158440"

---
MARKER : "1985_siggraph_19_245"
TYPE   : "in_journal"
AUTHOR : "Shoemake, K."
TITLE  : "Animating rotation with quaternion curves"
SERIAL : "ACM Siggraph Computer Graphics"
VOLUME : "19 (3)"
PAGE   : "245-254"
YEAR   : "1985-07"
DOI    : "10.1145/325165.325242"
TOPKEY : "ephemeris"
ABS    : "Solid bodies roll and tumble through space. In computer animation, so do cameras. The rotations of these objects are best described using a four coordinate system, quaternions, as is shown in this paper. Of all quaternions, those on the unit sphere are most suitable for animation, but the question of how to construct curves on spheres has not been much explored. This paper gives one answer by presenting a new kind of spline curve, created on a sphere, suitable for smoothly in-hetweening (i.e. interpolating) sequences of arbitrary rotations. Both theory and experiment show that the motion generated is smooth and natural, without quirks found in earlier methods."

---
MARKER : "1985_solar_phys_97_113"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z., Poletto, G."
TITLE  : "Hard X-ray images of possible reconnection in the flare of 21 May, 1980"
SERIAL : "Solar Phys."
VOLUME : "97 (1)"
PAGE   : "113-129"
YEAR   : "1985-05"
DOI    : "10.1007/BF00152982"

---
MARKER : "1984_asr_04_323"
TYPE   : "in_proceedings"
AUTHOR : "Hick, P., Stevens, G."
TITLE  : "The time scales of the scattering of energetic protons in interplanetary space"
EDITOR : "Koch-Miramond, M., Lee, M.A."
CTITLE : "COSPAR Symp. on Particle acceleration processes, shockwaves, nucleosythesis and cosmic rays"
SERIAL : "Adv. Space Res."
VOLUME : "4 (2/3)"
PAGE   : "323-326"
YEAR   : "1984-06"
DOI    : "10.1016/0273-1177(84)90328-4"
PLACE  : "Graz, AT, June 25-July 7, 1984"
TOPKEY : "interplanetary shocks"
ABS    : "Observations with the directional spectrometer DFH on-board ISEE 3 have been used to obtain results on the scattering time scales of energetic protons. Depending on the duration of the scattering process the particle distribution will be subjected to either phase scattering or full scattering. An analysis of some representative events shows that full scattering is applicable to shock-associated events."

---
MARKER : "1984_solar_phys_90_205"
TYPE   : "in_journal"
AUTHOR : "Neckel, H., Labs, D."
TITLE  : "The solar radiation between 300 and 12500 &Aring;"
SERIAL : "Solar Physics"
VOLUME : "90 (2)"
PAGE   : "205-258"
YEAR   : "1984-02"
DOI    : "10.1007/BF00173953"
TOPKEY : "solar radiation"
ABS    : "The results are based on absolute measurements of the disk-center intensities made more than 20 years ago and on Fourier transform spectra. A homogeneous and consistent set of absolute radiation data with high internal accuracy is derived for these FTS spectra. With a standard deviation of less than 0.2 percent, the maximum errors to be expected are of the order of 0.5 percent. This value is also seen as the upper limit for a neutral scale error, which may affect the overall irradiance integral (solar constant), and for systematic deviations occurring in relatively short spectral regions owing to the limited accuracy of the calibration curves. It is pointed out, however, that the overall spectral distribution cannot be seriously affected by systematic errors. This conclusion derives from the fact that the solar irradiance distribution agrees within observational errors with the flux distributions observed by Hardorp (1980) for solar-type stars (Neckel and Labs, 1981)."

---
MARKER : "1984_ssr_39_255"
TYPE   : "in_journal"
AUTHOR : "Burlaga, L.R."
TITLE  : "MHD processes in the outer heliosphere"
SERIAL : "Space Sci. Rev."
VOLUME : "39 (3/4)"
PAGE   : "255"
YEAR   : "1984-11"
DOI    : "10.1007/BF00173902"
TOPKEY : "MHD"

---
MARKER : "1984_solar_phys_94_427"
TYPE   : "in_journal"
AUTHOR : "Valnicek, B., Svestka, Z."
TITLE  : "Book reviews"
SERIAL : "Solar Phys."
VOLUME : "94 (2)"
PAGE   : "427"
YEAR   : "1984-09"
DOI    : "10.1007/BF00151328"
REMARK : "book review"

---
MARKER : "1984_solar_phys_94_171"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Revivals of a coronal arch"
SERIAL : "Solar Phys."
VOLUME : "94 (1)"
PAGE   : "171-192"
YEAR   : "1984-08"
DOI    : "10.1007/BF00154819"

---
MARKER : "1984_solar_phys_90_331"
TYPE   : "in_journal"
AUTHOR : "Dwivedi, B.N., Hudson, H.S., Kane, S.R., Svestka, Z."
TITLE  : "H_alfa and hard X-ray development in two-ribbon flares"
SERIAL : "Solar Phys."
VOLUME : "90 (2)"
PAGE   : "331-341"
YEAR   : "1984-02"
DOI    : "10.1007/BF00173961"

---
MARKER : "1984_adv_space_res_4_179"
TYPE   : "in_proceedings"
TITLE  : "Post-flare thermal waves in the solar corona"
AUTHOR : "Svestka, Z."
SERIAL : "Adv. Space Res."
VOLUME : "4 (7)"
PAGE   : "179-182"
YEAR   : "1984-00"
DOI    : "10.1016/0273-1177(84)90178-9"

---
MARKER : "1984_adv_space_res_4_287"
TYPE   : "in_proceedings"
TITLE  : "Imaging of reconnection processes in hard X-rays"
AUTHOR : "Svestka, Z., Poletto, G."
SERIAL : "Adv. Space Res."
VOLUME : "4 (7)"
PAGE   : "287-290"
YEAR   : "1984-00"
DOI    : "10.1016/0273-1177(84)90199-6"

---
MARKER : "1984_mem_soc_astron_italiana_55_725"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Large post-flare arch-like structures in the solar corona"
SERIAL : "Memorie della Societa Astronomica Italiana"
VOLUME : "55 (4)"
PAGE   : "725-36"
YEAR   : "1984-00"

---
MARKER : "1983_solar_phys_89_287"
TYPE   : "in_journal"
AUTHOR : "Schadee, A., de Jager, C., Svestka, Z."
TITLE  : "Enhanced X-ray emission above 3.5 keV in active regions in the absence of flares"
SERIAL : "Solar Phys."
VOLUME : "89 (2)"
PAGE   : "287-305"
YEAR   : "1983-12"
DOI    : "10.1007/BF00217252"

---
MARKER : "1983_solar_phys_88_315"
TYPE   : "in_journal"
AUTHOR : "Kattenberg, A., Allaart, M., de Jager, C., Schadee, A., Schrijver, J., Shibasaki, K., Svestka, Z., van Tend, W."
TITLE  : "Radio, X-ray, and optical observations of the flare of June 13, 1980, at 6h22m UT"
SERIAL : "Solar Phys."
VOLUME : "88 (1-2)"
PAGE   : "315-327"
YEAR   : "1983-10"
DOI    : "10.1007/BF00196195"

---
MARKER : "1983_solar_phys_87_271"
TYPE   : "in_journal"
AUTHOR : "Spicer, D.S., Svestka, Z."
TITLE  : "Transient brightenings of interconnecting loops"
SERIAL : "Solar Phys."
VOLUME : "87 (2)"
PAGE   : "271-278"
YEAR   : "1983-09"
DOI    : "10.1007/BF00224840"

---
MARKER : "1983_aa_125_150"
TYPE   : "in_journal"
AUTHOR : "Newhall, X.X., Standish, E.M., Williams, J.G."
TITLE  : "DE 102 - A numerically integrated ephemeris of the moon and planets spanning forty-four centuries"
SERIAL : "Astron. Astrophysics"
VOLUME : "125 (1)"
PAGE   : "150-167"
YEAR   : "1983-08"
TOPKEY : "ephemeris"
ABS    : "An ephemeris of the Moon and nine planets has been numerically integrated from 1411 BC to 3002 AD. The initial conditions for the simultaneous integration were based on fits to modern position measurements of the eight major planets and the Moon. The data include optical meridian transits, radar ranges, planetary spacecraft positions, and lunar laser ranges. The acceleration model for the integration is described and it is shown that the stability of the lunar integration depends upon simultaneously integrating the physical librations. A long ephemeris has utility for comparisons with both historical observations and analytical theories. Comparison with numerical representations permits the equinox and obliquity of the ephemeris to be recovered. At B1950.0 we find &eps;=24&deg;26'44''.816&plusmn;0''.015, which is 0''039 smaller than the presently adopted 1 AU value. Among the other determined parameters are the length of the astronomical unit, 149,597,870.68&plusmn;0.03 km. As newer, short ephemerides will continue to improve upon the accuracy of DE102, analytical corrections can be provided over the long span of DE102."

---
MARKER : "1983_solar_phys_86_267"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z., Schadee, A."
TITLE  : "Pre- and post-flare X-ray variations in active regions"
SERIAL : "Solar Phys."
VOLUME : "86 (1-2)"
PAGE   : "267-277"
YEAR   : "1983-07"
DOI    : "10.1007/BF00157200"

---
MARKER : "1983_space_sci_rev_35_259"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Post-flare coronal arches"
SERIAL : "Space Sci. Rev."
VOLUME : "35 (3)"
PAGE   : "259-267"
YEAR   : "1983-07"

---
MARKER : "1983_solar_phys_85_313"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z., Schrijver, J., Somov, B., Dennis, B.R., Woodgate, B.E., Fürst, E., Hirth, W., Raoult, A."
TITLE  : "Purely coronal flare-like variations"
SERIAL : "Solar Phys."
VOLUME : "85 (2)"
PAGE   : "313-337"
YEAR   : "1983-06"
DOI    : "10.1007/BF00148657"

---
MARKER : "1983_solar_phys_84_205"
TYPE   : "in_journal"
AUTHOR : "de Jager, C., Machado, M.E., Schadee, A., Strong, K.T., Svestka, Z., Woodgate, B.E., van Tend, W."
TITLE  : "The Queens' flare: Its structure and development; precursors, pre-flare brightenings, and aftermaths"
SERIAL : "Solar Phys."
VOLUME : "84 (1-2)"
PAGE   : "205-235"
YEAR   : "1983-04"
DOI    : "10.1007/BF00157457"

---
MARKER : "1983_publ_obs_ebro_mem_69"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Particle acceleration in two-ribbon flares"
SERIAL : "Publ. Obs. Ebro Mem."
VOLUME : "14"
PAGE   : "69-81"
YEAR   : "1983-00"

---
MARKER : "1983_adv_space_res_2"
TYPE   : "proceedings"
EDITOR : "Svestka, Z., Rust, D.M., Dryer, M."
TITLE  : "Solar Maximum Year"
PLACE  : "COSPAR 24, Ottawa, Canada, 16 May-2 June 1982"
SERIAL : "Adv. Space Res."
VOLUME : "2 (11)"
PAGE   : "(7+294 pages)"
YEAR   : "1983-00"

---
MARKER : "1982_aa_114_297"
TYPE   : "in_journal"
AUTHOR : "Standish, E.M."
TITLE  : "Orientation of the JPL Ephemerides, DE 200/LE 200, to the dynamical equinox of J 2000"
SERIAL : "Astron. Astrophys."
VOLUME : "114 (2)"
PAGE   : "297-302"
YEAR   : "1982-10"
TOPKEY : "ephemeris"
ABS    : "The lunar and planetary ephemerides, DE200/LE2100 have been recently produced at JPL. They will form the basis of the ephemerides in the 'Astronomical Almanac' starting in the year 1984. The origin has been referenced to the J2000 dynamical equinox of the ephemerides themselves. The procedure for this orientation is described here in detail. Analyses of the ephemerides also provide comparisons with the equinox of the FK4 and with presently adopted values for the Earth's obliquity"

---
MARKER : "1982_solar_phys_80_143"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z., Dennis, B.R., Pick, M., Raoult, A., Rapley, C.G., Stewart, R.T., Woodgate, B.E."
TITLE  : "Unusual coronal activity following the flare of 6 November 1980"
SERIAL : "Solar Phys."
VOLUME : "80 (1)"
PAGE   : "143-159"
YEAR   : "1982-09"
DOI    : "10.1007/BF00153429"

---
MARKER : "1982_aa_110_355"
TYPE   : "in_journal"
AUTHOR : "Leinert, C., Richter, I., Pitz, E., Hanner, M."
TITLE  : "Helios zodiacal light measurements - A tabulated summary"
SERIAL : "Astron. Astrophys."
VOLUME : "110"
PAGE   : "355"
YEAR   : "1982-06"
TOPKEY : "Helios photometers, zodiacal light"
ABS    : "Intensity, colour and polarization of the average zodiacal light as observed by the Helios zodiacal light experiment between December 1974 and January 1981 are given in tabulated form."

---
MARKER : "1982_aa_110_111"
TYPE   : "in_journal"
AUTHOR : "Leinert, C., Richter, I., Planck, B."
TITLE  : "Stability of the zodiacal light from mimimum to maximum of the solar cycle (1974-1981)"
SERIAL : "Astron. Astrophys."
VOLUME : "110"
PAGE   : "111-114"
YEAR   : "1982-06"
TOPKEY : "Helios photometers, zodiacal light"
ABS    : "In order to demonstrate the stability of zodiacal light, observations made with the Helios 1 and 2 space probes over the time interval December 1974 through July 1981 are presented. This interval covers the rising part of solar cycle 21, characterized by a very quiet minimum in June 1976 and a quite strong maximum in November 1979. Data evidencing the stability of the photometers is shown, along with an example from the data base from which the results are derived. The stability of zodical light intensity and polarization is also depicted. It is concluded that two percent for the intensity and 0.01 for polarization are reasonable upper limits for a suspected solar cycle variation, showing that the interplanetary particles producing the zodiacal light are at most weakly influenced by interplanetary plasma and magnetic fields. It is hypothesized that the zodiacal light, if properly measured, is a stable reference."

---
MARKER : "1982_solar_phys_78_271"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z., Dodson-Prince, H.W., Martin, S.F., Mohler, O.C., Moore, R.L., Nolte, J.T., Petrasso, R.D."
TITLE  : "Study of the post-flare loops on 29 July 1973, IV. Revision of T and n_e values and comparison with the flare of 21 May 1980"
SERIAL : "Solar Phys."
VOLUME : "78 (2)"
PAGE   : "271-285"
YEAR   : "1982-06"
DOI    : "10.1007/BF00151609"

---
MARKER : "1982_solar_phys_75_305"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z., Stewart, R.T., Hoyng, P., van Tend, W., Acton, L.W., Gabriel, A.H., Rapley, C.G., Boelee, A., Bruner, E.C., de Jager, C., Lafleur, H., Nelson, G., Simnett, G.M., van Beek, H.F., Wagner, W.J."
TITLE  : "Observations of a post-flare radio burst in X-rays"
SERIAL : "Solar Phys."
VOLUME : "75 (1-2)"
PAGE   : "305-329"
YEAR   : "1982-01"
DOI    : "10.1007/BF00153479"

---
MARKER : "1982_adv_space_res_2_3"
TYPE   : "in_proceedings"
TITLE  : "Flare build-up study in the SMA period"
AUTHOR : "Svestka, Z."
SERIAL : "Adv. Space Res."
VOLUME : "2 (11)"
PAGE   : "3-4"
YEAR   : "1982-00"
DOI    : "10.1016/0273-1177(82)90172-7"

---
MARKER : "1981_aas_46_115"
TYPE   : "in_journal"
AUTHOR : "Leinert, C., Richter, I."
TITLE  : "UBV surface brightness photometry of eight sections through the Milky Way from the Helios space probes"
SERIAL : "Astron. Astrophys. Suppl. Ser."
VOLUME : "46"
PAGE   : "115-129"
YEAR   : "1981-10"
TOPKEY : "Helios photometers"
ABS    : "The zodiacal light experiment on Helios measures the brightness of the Milky Way along four strips of constant ecliptical latitude. In extension of earlier work UBV brightnesses were obtained for all of the resulting eight sections through the Milky Way. When comparing them to available photometries the agreement is reasonably good with Pfleiderer and Mayer in U, with Elsaesser and Haug in V, and particularly close with Classen in B. The Helios results support the U-B and B-V colors predicted from Mattila's synthetic Milky Way model. They also suggest that the intensity of the interstellar radiation field is decreasing from V to U."

---
MARKER : "1981_solar_phys_71_349"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z., Howard, R."
TITLE  : "Transient brightenings of interconnecting loops"
SERIAL : "Solar Phys."
VOLUME : "71 (2)"
PAGE   : "349-359"
YEAR   : "1981-06"
DOI    : "10.1007/BF00167557"

---
MARKER : "1981_apjl_246_l155"
TYPE   : "in_journal"
AUTHOR : "Hoyng, P., Duijveman, A., Machado, M.E., Rust, D.M., Svestka, Z., Boelee, A., de Jager, C., Frost, K.J., Lafleur, H., Simnett, G.M., Van Beek, H.F., Woodgate, B.E."
TITLE  : "Origin and location of the hard X-ray emission in a two-ribbon flare"
SERIAL : "Astrophys. J. Lett."
VOLUME : "246 (3)"
PAGE   : "L155-L159"
YEAR   : "1981-06"

---
MARKER : "1981_solar_phys_71_49"
TYPE   : "in_journal"
AUTHOR : "Howard, R., Svestka, Z."
TITLE  : "On the outburst of flare activity of 26 November, 1973"
SERIAL : "Solar Phys."
VOLUME : "71 (1)"
PAGE   : "49-53"
YEAR   : "1981-05"
DOI    : "10.1007/BF00153605"

---
MARKER : "1981_apjl_244_l157"
TYPE   : "in_journal"
AUTHOR : "Van Beek, H.F., de Jager, C., Fryer, R., Schadee, A., Svestka, Z., Boelee, A., Duijveman, A., Galama, M., Hoekstra, R., Hoyng, P., Imhof, J.P., Lafleur, H., Machado, M.E., Maseland, H.V.A.M., Mels, W.A., Schrijver, J., Simnett, G.M., van der Laan, J.J.M., van Rens, P., van Tend, W., Werkhoven, F., Willmore, A.P., Wilson, J.W.G., Zandee, W."
TITLE  : "The limb flare of 1980 April 30 as seen by the Hard X-ray Imaging Spectrometer"
SERIAL : "Astrophys. J. Lett"
VOLUME : "244 (3)"
PAGE   : "L157-L162"
YEAR   : "1981-05"

---
MARKER : "1981_apjl_244_l153"
TYPE   : "in_journal"
AUTHOR : "Hoyng, P., Machado, M.E., Duijveman, A., Boelee, A., de Jager, C., Fryer, R., Galama, M., Hoekstra, R., Imhof, J., Lafleur, H., Maseland, H.V.A.M., Mels, W.A., Schadee, A., Schrijver, J., Simnett, G.M., Svestka, Z., van Beek, H.F., van Tend, W., van der Laan, J.J.M., van Rens, P., Werkhoven, F., Willmore, A.P., Wilson, J.W.G., Zandee, W."
TITLE  : "Hard X-ray imaging of two flares in active region 2372"
SERIAL : "Astrophys. J. Lett"
VOLUME : "244 (3)"
PAGE   : "L153-L156"
YEAR   : "1981-03"

---
MARKER : "1981_solar_phys_72_vii"
TYPE   : "in_journal"
AUTHOR : "de Jager, C., Švestka, Z."
TITLE  : "Introduction: index Vol. 1-55"
SERIAL : "Solar Phys."
VOLUME : "72 (1-2)"
PAGE   : "vii"
YEAR   : "1981-03"
DOI    : "10.1007/BF00157135"

---
MARKER : "1981_solar_phys_69_419"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Book review"
SERIAL : "Solar Phys."
VOLUME : "69 (2)"
PAGE   : "419"
YEAR   : "1981-02"
DOI    : "10.1007/BF00150006"
REMARK : "book review"

---
MARKER : "1981_fmag_solar_flare_mhd"
TYPE   : "in_book"
AUTHOR : "Svestka, Z."
TITLE  : "Flare observations"
EDITOR : "Priest, E.R."
CTITLE : "Solar flare magnetohydrodynamics"
SERIAL : "Fluid mechanics of astrophysics and geophysics"
VOLUME : "1"
CHAPTER: "2"
PAGE   : "47-138"
YEAR   : "1981-00"
PUBLISH: "Gordon and Breach"

---
MARKER : "1981_adv_space_res_1_251"
TYPE   : "in_proceedings"
TITLE  : "Structural development of the X-ray limb flare of 30 April 1980"
AUTHOR : "de Jager, C., Hoyng, P., Lafleur, H., Schadee, A., Svestka, Z., van Beek, H.F., van Tend, W., Fryer, R., Simnett, G.M."
SERIAL : "Adv. Space Res."
VOLUME : "1 (13)"
PAGE   : "251-254"
YEAR   : "1981-00"
DOI    : "10.1016/0273-1177(81)90205-2"

---
MARKER : "1981_adv_space_res_1_255"
TYPE   : "in_proceedings"
TITLE  : "Solar maximum mission experiment: early results of the hard X-ray imaging experiment"
AUTHOR : "Boelee, A., de Jager, C., Duijveman, A., Galama, M., Hoekstra, R., Hoyng, P., Imhof, J.P., Lafleur, H., Maseland, H.V.A.M., Mels, W.A., Schadee, A., Schrijver, J., Svestka, Z., van Beek, H.F., van Rens, P., van der Laan, J.J.M., van Tend, W., Werkhoven, F., Wiersma, G., Zandee, W., Simnett, G.M., Charlton, C.P., Fryer, R., Willmore, A.P., Wilson, J.W.G., Machado, M.E."
SERIAL : "Adv. Space Res."
VOLUME : "1 (13)"
PAGE   : "255-266"
YEAR   : "1981-00"
DOI    : "10.1016/0273-1177(81)90206-4"

---
MARKER : "1980_solar_phys_67_379"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z., Hoven, G., Hoyng, P., Kuperus, M."
TITLE  : "Brief report of the meeting"
SERIAL : "Solar Phys."
VOLUME : "67 (2)"
PAGE   : "379-384"
YEAR   : "1980-08"
DOI    : "10.1007/BF00149814"

---
MARKER : "1980_space_sci_rev_26_317"
TYPE   : "in_proceedings"
AUTHOR : "Svestka, Z., de Jager, C."
TITLE  : "The solar maximum year and related space experiments"
CTITLE : "22^nd COSPAR meeting, 7 June 1979, Bangalore, India"
SERIAL : "Space Sci. Rev."
VOLUME : "26"
PAGE   : "317-330"
YEAR   : "1980-07"

---
MARKER : "1980_phil_trans_royal_soc_london_297_575"
TYPE   : "in_proceedings"
AUTHOR : "Svestka, Z."
TITLE  : "Activated solar filements and flares"
SERIAL : "Phil. Trans. Royal Soc. London, Series A"
VOLUME : "297 (1433)"
PAGE   : "575-585"
YEAR   : "1980-07"
URL    : "http://adsabs.harvard.edu/abs/1980RSPTA.297..575S"

---
MARKER : "1980_solar_flares_341"
TYPE   : "in_proceedings"
AUTHOR : "Moore, R.L., McKenzie, D.L., Svestka, Z.,Widing, K.G., Antiochos, S.K., Dere, K.P., Dodson-Prince, H.W., Hiei, E., Krall, K.R., Krieger, A.S., Mason, H.E., Petrasso, R.D., Pneuman, G.W., Silk, J.K., Vorpahl, J.A., Withbroe, G.L."
TITLE  : "The thermal X-ray flare plasma"
CTITLE : "Solar Flares, a monograph from Skylab Solar Workshop II"
EDITOR : "Sturrock, P.A."
PAGE   : "341-409"
YEAR   : "1980-00"
PUBLISH: "Colorado Ass. Univ. Press, Boulder"
URL    : "http://adsabs.harvard.edu/abs/1980sfsl.work..341M"

---
MARKER : "1980_solar_interplanetary_dynamics_217"
TYPE   : "in_proceedings"
AUTHOR : "Svestka, Z., Martin, S.F., Kopp, R.A."
TITLE  : "Particle acceleration in the process of eruptive opening and reconnection of magnetic fields"
CTITLE : "Proc. Symp. on Solar and interplanetary dynamics"
EDITOR : "Dryer, M., Tandberg-Hanssen, E."
PLACE  : "Cambridge, MA, US, 27-31 August 1979"
PAGE   : "217-221"
YEAR   : "1980-00"
DOI    : "10.1007/978-94-009-9100-2_34"
ABS    : "In a series of papers on the flare of 29 July 1973 (Nolte et al., 1979; Martin, 1979; Svestka et al., 1979) it has been shown that Halfa 'post-flare' loops are the cooled aftermath of previously hot coronal loops which were visible in x-rays in the same position earlier in the flare. Kopp and Pneuman (1976) have proposed that these post-flare loops are formed by a process of successive magnetic field reconnections of previously distended magnetic field lines as illustrated in Figure 1. Each successive reconnection of the magnetic field yields a closed magnetic loop that forms above and concentric with previously formed loops. A shock wave created during each sudden reconnection travels down both legs of each loop and provides energy for ionizing chromospheric mass at the footpoints of the loop. Subsequent condensation of the ionized mass at the tops of the loops renders them visible as this mass falls to the chromosphere."

---
MARKER : "1980_mitt_astron_gesellschaft_50_96"
TYPE   : "in_journal"
AUTHOR : "Kittelberger, G., Elwert, G., Svestka, Z."
TITLE  : "Gibt es Cluster von hellen Punkten?"
SERIAL : "Mitteilungen der Astronomischen Gesellschaft"
VOLUME : "50"
PAGE   : "96-97"
YEAR   : "1980-00"
URL    : "http://adsabs.harvard.edu/abs/1980MitAG..50...96K"

---
MARKER : "1979_soltip_2_322"
TYPE   : "in_proceedings"
AUTHOR : "Svestka, Z."
TITLE  : "The needs for prediction and real-time monitoring for the flare build-up study"
CTITLE : "Proc. on Solar-terrestrial Predictions"
VOLUME : "2"
PAGE   : "322-330"
YEAR   : "1979-12"

---
MARKER : "1979_solar_phys_63_279"
TYPE   : "in_journal"
AUTHOR : "Rust, D.M., Svestka, Z."
TITLE  : "Slowly moving disturbances in the X-ray corona"
SERIAL : "Solar Phys."
VOLUME : "63 (2)"
PAGE   : "279-295"
YEAR   : "1979-09"
DOI    : "10.1007/BF00174535"

---
MARKER : "1979_solar_phys_63_105"
TYPE   : "in_journal"
AUTHOR : "Howard, R., Fritzova-Svestkova, L., Svestka, Z."
TITLE  : "The birthplaces of active regions and X-ray bright points"
SERIAL : "Solar Phys."
VOLUME : "63 (1)"
PAGE   : "105-111"
YEAR   : "1979-08"
DOI    : "10.1007/BF00155700"

---
MARKER : "1979_solar_phys_63_297"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z., Howard, R."
TITLE  : "Transient brightenings of interconnecting loops"
SERIAL : "Solar Phys."
VOLUME : "63 (2)"
PAGE   : "297-318"
YEAR   : "1979-09"
DOI    : "10.1007/BF00174536"

---
MARKER : "1979_solar_phys_62_123"
TYPE   : "in_journal"
AUTHOR : "Nolte, J.T., Gerassimenko, M., Krieger, A.S., Petrasso, R.D., Svestka, Z."
TITLE  : "Study of the post-flare loops on 29 July 1973, I: Dynamics of the X-ray loops"
SERIAL : "Solar Phys."
VOLUME : "62 (1)"
PAGE   : "123-132"
YEAR   : "1979-05"
DOI    : "10.1007/BF00150139"

---
MARKER : "1979_solar_phys_62_133"
TYPE   : "in_journal"
AUTHOR : "Petrasso, R.D., Nolte, J.T., Gerassimenko, M., Krieger, A.S., Krogstad, R., Seguin, F.H., Svestka, Z."
TITLE  : "Study of the post-flare loops on 29 July 1973, II: Physical parameters in the X-ray loops"
SERIAL : "Solar Phys."
VOLUME : "62 (1)"
PAGE   : "133-144"
YEAR   : "1979-05"
DOI    : "10.1007/BF00150140"

---
MARKER : "1979_phys_solar_prominences_357"
TYPE   : "in_proceedings"
AUTHOR : "Svestka, Z."
TITLE  : "Prominences and solar activity"
CTITLE : "Proc. IAU Coll. 44 on Physics of solar prominences"
PLACE  : "Oslo, Norway, 14-18 August 1978"
PAGE   : "357-372"
YEAR   : "1979-00"

---
MARKER : "1979_phys_solar_prominences_276"
TYPE   : "in_proceedings"
AUTHOR : "Rust, D.M., Svestka, Z."
TITLE  : "Slowly-moving disturbances in the X-ray corona"
CTITLE : "Proc. IAU Coll. 44 on Physics of solar prominences"
PLACE  : "Oslo, Norway, 14-18 August 1978"
PAGE   : "276-277"
YEAR   : "1979-00"

---
MARKER : "1978_solar_phys_60_3"
TYPE   : "in_journal"
AUTHOR : "de Jager, C., Svestka, Z."
TITLE  : "An editorial note"
SERIAL : "Solar Phys."
VOLUME : "60 (1)"
PAGE   : "3"
YEAR   : "1978-11"
DOI    : "10.1007/BF00152327"
REMARK : "editorial"

---
MARKER : "1978_closeup_sun_234"
TYPE   : "in_proceedings"
AUTHOR : "Stevens, G.A., van Rooijen, J.J., Svestka, Z., De Jager, C."
TITLE  : "Low-energy protons: gradients in interplanetary space and distribution in the solar corona"
CTITLE : "JPL A close-up of the Sun"
PAGE   : "234-239"
YEAR   : "1978-09"
URL    : "http://adsabs.harvard.edu/abs/1978clus.nasa..234S"
ABS    : "First and second order anisotropy measurements are proposed as a tool for studying the coronal source function and interplanetary propagation of low energy protons. Optimum orbit and attitude requirements are suggested for a three telescope system. Some limitations with regard to the lower energy limit for a feasible set-up are discussed."

---
MARKER : "1978_solar_phys_57_483"
TYPE   : "book_review"
AUTHOR : "Svestka, Z."
TITLE  : "Book review"
SERIAL : "Solar Phys."
VOLUME : "57 (2)"
PAGE   : "483"
YEAR   : "1978-04"
DOI    : "10.1007/BF00160121"
REMARK : "book review"

---
MARKER : "1978_solar_phys_56_471"
TYPE   : "in_journal"
AUTHOR : "Howard, R., Svestka, Z."
TITLE  : "Erratum: 'Development of a complex of activity in the solar corona' [Sol. Phys., Vol. 54, p. 65 - 105 (1977)]"
SERIAL : "Solar Phys."
VOLUME : "56 (2)"
PAGE   : "471"
YEAR   : "1978-02"
DOI    : "10.1007/BF00152487"

---
MARKER : "1978_solar_phys_56_3"
TYPE   : "in_journal"
AUTHOR : "de Jager, C., Svestka, Z."
TITLE  : "Editorial"
SERIAL : "Solar Phys."
VOLUME : "56 (1)"
PAGE   : "3-4"
YEAR   : "1978-01"
DOI    : "10.1007/BF00152629"
REMARK : "editorial"

---
MARKER : "1977_solar_phys_55_401"
TYPE   : "in_journal"
AUTHOR : "Nolte, J.T., Gerassimenko, M., Krieger, A.S., Petrasso, R.D., Svestka, Z., Wentzel, D.G."
TITLE  : "Do changes in coronal emission structure imply magnetic reconnection?"
SERIAL : "Solar Phys."
VOLUME : "55 (2)"
PAGE   : "401-412"
YEAR   : "1977-12"
DOI    : "10.1007/BF00152583"
TOPKEY : "solar activity"
ABS    : "We examine three major possible interpretations of observed reconfigurations of coronal X-ray and X UV emitting structures on a scale comparable to the size of the structures themselves. One possibility is that little change in the large-scale magnetic field configuration is associated with the change in emission. The other two possibilities are processes by which the magnetic field structure can change. We demonstrate that large changes in visibility in X-rays or XUV lines can be associated with relatively minor changes in the coronal magnetic field by showing the behavior of magnetic interconnections between individual active regions in a complex of activity observed by the S-054 X-ray spectrographic telescope on Skylab. While the large-scale interconnections are continuously present for at least several days, individual loops in these structures are visible for only relatively short times (&le;1 day). The two theoretical possibilities which we discuss are 'frozen-in' motion of the fields, and field line reeonneetion. We emphasize that reconnection occurs in regions much smaller than telescopic resolution. Because there are no measurements of the magnetic field in the corona in projection against the disk, existing observations are generally not sufficient to show in detail ho~omuch reconnection has occurred."

---
MARKER : "1977_solar_phys_55_359"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z., Solodyna, C.V., Howard, R., Levine, R.H."
TITLE  : "Open magnetic fields in active regions"
SERIAL : "Solar Phys."
VOLUME : "55 (2)"
PAGE   : "359-369"
YEAR   : "1977-12"
DOI    : "10.1007/BF00152579"
TOPKEY : "solar activity"
ABS    : "Soft X-ray observations confirm that some of the dark gaps seen between interconnecting loops and inner cores of active regions may be loci of open fields, as it has been predicted by global potential extrapolation of photospheric magnetic fields. It seems that the field lines may open only in a later state of the active region development."

---
MARKER : "1977_physics_today_30_72"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z., Parker, E.N."
TITLE  : "Solar flares"
SERIAL : "Physics Today"
VOLUME : "30 (10)"
PAGE   : "72"
YEAR   : "1977-10"
DOI    : "10.1063/1.3037754"

---
MARKER : "1977_solar_phys_54_65"
TYPE   : "in_journal"
AUTHOR : "Howard, R., Svestka, Z."
TITLE  : "Development of a complex of activity in the solar corona"
SERIAL : "Solar Phys."
VOLUME : "54 (1)"
PAGE   : "65-105"
YEAR   : "1977-09"
DOI    : "10.1007/BF00146426"
TOPKEY : "solar activity"
ABS    : "Skylab observations of the Sun in soft X-rays gave us the first possibility to study the development of a complex of activity in the solar corona during its whole lifetime of seven solar rotations. The basic components of the activity complex were permanently interconnected (including across the equator) through sets of magnetic field lines, which suggests similar connections also below the photosphere. However, the visibility of individual loops in these connections was greatly variable and typically shorter than one day. Each brightening of a coronal loop in X-rays seems to be related to a variation in the photospheric magnetic field near its footpoint. Only loops (rarely visible) connecting active regions with remnants of old fields can be seen in about the same shape for many days. The interconnecting X-ray loops do not connect sunspots. We point out several examples of possible reconnections of magnetic field lines, giving rise to the onset of the visibility or, more likely, to sudden enhancements of the loop emission. In one case a new system of loops brightened in X-rays, while the field lines definitely could not have reconnected. Some striking brightenings show association with flares, but the flare occurrence and the loop brightening seem to be two independent consequences of a common triggering action: emergence of new magnetic flux. In old active regions, growing and/or brightened X-ray loops can be seen quite often without any associated flare; thus, the absence of any flaring in the chromosphere does not necessarily mean that the overlying coronal active region is quiet and inactive. We further discuss the birth of the interconnecting loops, their lifetime, altitude, variability in shape in relation to the photospheric magnetic field, the similarity of interconnecting and internal loops in the late stages of active regions, phases of development of an active region as manifested in the corona, the remarkably linear boundary of the X-ray emission after the major flare of 29 July 1973, and a striking sudden change in the large-scale pattern of unipolar fields to the north of the activity complex. The final decay of the complex of activity was accompanied by the penetration of a coronal hole into the region where the complex existed before."

---
MARKER : "1977_solar_phys_53_221"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Introductory talk, Part I: Magnetic configurations and instabilities in flares"
SERIAL : "Solar Phys."
VOLUME : "53 (1)"
PAGE   : "221-222"
YEAR   : "1977-07"
DOI    : "10.1007/BF02260222"
TOPKEY : "flares"

---
MARKER : "1977_solar_phys_52_229"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Book reviews"
SERIAL : "Solar Phys."
VOLUME : "52 (1)"
PAGE   : "229"
YEAR   : "1977-04"
DOI    : "10.1007/BF00935804"
REMARK : "book review"

---
MARKER : "1977_solar_phys_52_69"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z., Krieger, A.S., Chase, R.C., Howard, R."
TITLE  : "Transequatorial loops interconnecting McMath regions 12472 and 12474"
SERIAL : "Solar Phys."
VOLUME : "52 (1)"
PAGE   : "69-90"
YEAR   : "1977-04"
DOI    : "10.1007/BF00935791"
TOPKEY : "solar activity"
ABS    : "We discuss the life-story of a transequatorial loop system which interconnected the newly born active region McMath 12474 with the old region 12472. The loop system was probably born through reconnection accomplished 1.5 to 5 days after the birth of 12474 and the loops were observed in soft X-rays for at least 1.5 days. Transient 'sharpenings' of the interconnection and a striking brightening of the whole loop system for about 6 hr appear to be caused by magnetic field variations in the region 12474. A flare might have been related to the brightening, but only in an indirect way: the same emerging flux could have triggered the flare and at the same time strengthened the magnetic field at the foot-points of the loops. Electron temperature in the loop system, equal to 2.1&times;10<sup>6</sup> K in its quiet phase, increased to 3.1&times;10<sup>6</sup> K during the brightening. Electron density in the loop system was &le;1.3&times;10<sup>9</sup> cm<sup>-3</sup> and it could be estimated to ~7&times;10<sup>8</sup>cm<sup>-3</sup> prior to the brightening. During the brightening the loops became twisted. There was no obvious effect whatsoever of the activity in 12474 upon the in erconnected old region. The final decay of the loop system reflected the decay of magnetic field in the region 12474."

---
MARKER : "1976_solar_phys_50_491"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z., Fritzova-Svestkova, L., Nolte, J.T., Dodson-Prince, H.W., Hedeman, E.R."
TITLE  : "Low-energy particle events associated with sector boundaries"
SERIAL : "Solar Phys."
VOLUME : "50 (2)"
PAGE   : "491-500"
YEAR   : "1976-11"
DOI    : "10.1007/BF00155310"
TOPKEY : "solar particle events, sector boundaries"
ABS    : "Onsets of some 40 to 45 low-energy proton events during the years 1957 1969 coincided in time with transits of well-defined sector boundaries across the Earth. These events can be interpreted as long-lived proton streams filling up some of the magnetic sectors, indicating an acceleration of protons which is not associated with typical proton-producing flares. The sharp onsets of these particle streams, as well as a deficiency of flare-associated particle events shortly before the boundary transit, indicate that in some cases magnetic sector boundaries can inhibit transverse propagation of low-energy particles in the solar corona or in interplanetary space."

---
MARKER : "1976_solar_phys_48_275"
TYPE   : "in_journal"
AUTHOR : "Fritzova-Svestkova, L., Chase, R.C., Svestka, Z."
TITLE  : "On the occurrence of sympathetic flares"
SERIAL : "Solar Phys."
VOLUME : "48 (2)"
PAGE   : "275-286"
YEAR   : "1976-06"
DOI    : "10.1007/BF00151996"
TOPKEY : "flares"
ABS    : "We have tried to determine whether statistical evidence on the occurrence of sympathetic flares, which is negative for whole-disk data, can be found for particular, physically connected, pairs of active regions. Recently, Simnett (1974) and Gergely and Erickson (1975) claimed to have found such evidence, but their results were based on incorrect computations of the random incidence of flares. If the correct formula is applied, the supposed evidence disappears. The results are negative also for pairs of active regions interconnected with magnetic loops visible in soft X-rays during the Skylab mission. The only positive result (with statistical confidence of 3.4 &sigma;) is found for pairs of active regions, which are closer than 30&deg; to each other, without specifying any kind of physical relationship. For such pairs of regions the occurrence of short-time (&lt;20 min) intervals between flares is increased, but the time interval pattern does not correspond to any mode of propagation of a triggering agent in the solar atmosphere. Therefore, if the increase has real physical significance, it would be indicative of some kind of subphotospheric synchronization of activity in nearby 'sympathetic' active regions."

---
MARKER : "1976_phil_trans_royal_soc_london_281_435"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Optical observations of flares"
SERIAL : "Phil. Trans. Royal Soc. London A (Mathematical and Physical Sciences)"
VOLUME : "281 (1304)"
PAGE   : "435-441"
YEAR   : "1976-05"
TOPKEY : "flares"
URL    : "http://www.jstor.org/stable/74613"
ABS    : "The lecture describes solar flare effects in the chromosphere and photosphere, particularly emphasizing problems of the energy transfer, and the differences between  thermal and non-thermal phases of the flare development. Filamentary and shell models are compared and the depth of the white-light flare emission is discussed. Optical effects possibly associated with other, non-optical flare-associated phenomena are pointed out."

---
MARKER : "1976_gam_solar_flares"
TYPE   : "book"
AUTHOR : "Svestka, Z."
TITLE  : "Solar flares"
SERIAL : "Geophysics and Astrophysics Monographs"
PAGE   : "(415 pages)"
YEAR   : "1976-04"
PUBLISH: "D. Reidel Publ. Co., Dordrecht"

---
MARKER : "1976_solar_phys_47_375"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "What should be observed on the sun"
SERIAL : "Solar Phys."
VOLUME : "47 (1)"
PAGE   : "375-384"
YEAR   : "1976-03"
DOI    : "10.1007/BF00152276"
TOPKEY : "solar activity"
ABS    : "Three problems are emphasized in particular: the preflare magnetic field configuration, velocity fields, and the nature of acceleration processes in flares. It is concluded that what we need most urgently are high-resolution hard X-ray, soft X-ray, and EUV-pictures, coronal spectra, and magnetograms with high resolution both in space and time. A space-shuttle equipped with instrumentation of this kind would contribute significantly to our knowledge of the flare process"

---
MARKER : "1976_solar_phys_47_9"
TYPE   : "in_journal"
AUTHOR : "de Jager, C., Obayashi, T., Svestka, Z."
TITLE  : "Preface topical issue 'Flare Build-up Study'"
SERIAL : "Solar Phys."
VOLUME : "47 (1)"
PAGE   : "9"
YEAR   : "1976-03"
DOI    : "10.1007/BF00152239"
TOPKEY : "flares"

---
MARKER : "1976_lnp_48_19"
TYPE   : "in_proceedings"
AUTHOR : "Pitz, E., Leinert, C., Link, H., Salm, N."
TITLE  : "Helios zodiacal light experiment"
EDITOR : "Ehlers, J., Hepp, K., Weidenmeller, H.A., Zittartz, J."
CTITLE : "IAU Coll. 31 on Interplanetary Dust and Zodiacal Light"
SERIAL : "Lecture Notes in Physics"
VOLUME : "48"
PAGE   : "19-23"
YEAR   : "1976-00"
DOI    : "10.1007/3-540-07615-8_446"
TOPKEY : "Helios photometers"
PLACE  : "Heidelberg, Germany, 10-13 June 1975"
ABS    : "No abstract in paper"

---
MARKER : "1976_space_research_xvi_917"
TYPE   : "in_proceedings"
AUTHOR : "Chase, R.C., Krieger, A.S., Svestka, Z., Vaiana, G.S."
TITLE  : "SKYLAB observations of X-ray loops connecting separate active regions"
CTITLE : "Space Research XVI, Proc. Open Meetings of Working Groups on Physical Sciences (May 29-June 7, 1975), and Symposium and Workshop on Results from Coordinated Upper Atmosphere Measurement Programs"
PLACE  : "Varna, Bulgaria, 29-31 May 1975"
EDITOR : "Rycroft, M.J."
PAGE   : "917-922"
YEAR   : "1976-00"
PUBLISH: "Akademie-Verlag GmbH"
TOPKEY : "solar activity"
URL    : "http://adsabs.harvard.edu/abs/1976spre.conf..917C"
ABS    : "One hundred loops interconnecting 94 separate active solar regions detectable in soft X-rays were identified during the Skylab mission. While close active regions are commonly interconnected with loops, the number of such interconnections decreases steeply for longer distances; the longest interconnecting loop observed in the Skylab data connected regions separated by 37 deg. Several arguments are presented which support the point of view that this is the actual limit of the size of magnetic interconnections between active regions. No sympathetic flares could be found in the interconnected regions. These results cast doubt on the hypothesis that accelerated particles can be guided in interconnecting loops from one active region to another over distances of 100 deg or more and eventually produce sympathetic flares in them."

---
MARKER : "1976_lnp_48_24"
TYPE   : "in_proceedings"
AUTHOR : "Link, H., Leinert, C., Pitz, E., Salm, N."
TITLE  : "Preliminary results of the Helios A zodiacal light experiment"
EDITOR : "Ehlers, J., Hepp, K., Weidenmeller, H.A., Zittartz, J."
CTITLE : "IAU Coll. 31 on Interplanetary Dust and Zodiacal Light"
SERIAL : "Lecture Notes in Physics"
VOLUME : "48"
PAGE   : "24-28"
YEAR   : "1976-00"
DOI    : "10.1007/3-540-07615-8_447"
TOPKEY : "Helios photometers"
PLACE  : "Heidelberg, Germany, 10-13 June 1975"
ABS    : "No abstract in paper"

---
MARKER : "1976_russian_126"
TYPE   : "in_proceedings"
AUTHOR : "Svestka, Z."
TITLE  : "Several aspects of flare-associated particle events"
CTITLE : "Nablyud. i prognoz soln. aktivnosti. Moskva, Mir"
PAGE   : "126-144"
YEAR   : "1976-00"
TOPKEY : "flares, solar particle events"
URL    : "http://adsabs.harvard.edu/abs/1976npsa.conf..126S"

---
MARKER : "1976_trans_iau_16a_13"
TYPE   : "in_journal"
AUTHOR : "Newkirk, G., Dunn, R.B., Mehltretter, P., MacQueen, R., Bonnet, R.M., White, O.R., Fokker, A.D., Zwaan, C., Bruzek, A., Durrant, C., Grossmann-Doerth, U., Mehltretter, J.P., Svestka, Z., de Feiter, L.D., Tandberg-Hanssen, E., Howard, R., Stix, M., Pneuman, G.W., Hundhausen, A.J., Sawyer, C., Simon, P."
TITLE  : "Solar activity (Activite solaire)"
SERIAL : "Trans. Int. Astron. Union (Reports on Astronomy)"
VOLUME : "16A (2)"
PAGE   : "13-54"
YEAR   : "1976-00"
TOPKEY : "solar activity"
URL    : "http://adsabs.harvard.edu/abs/1976IAUTA..16b..13N"

---
MARKER : "1975_solar_phys_45_543"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Book review"
SERIAL : "Solar Phys."
VOLUME : "45 (2)"
PAGE   : "543"
YEAR   : "1975-12"
DOI    : "10.1007/BF00158469"
REMARK : "book review"

---
MARKER : "1976_soltip_1_129"
TYPE   : "in_proceedings"
AUTHOR : "Williams, D.J., Svestka, Z."
TITLE  : "Development of solar active regions"
CTITLE : "Proc. Intl Symp. on Solar-Terrestrial Physics 'Physics of solar planetary environments'"
PLACE  : "Boulder, CO, US, 7-18 June 1976"
VOLUME : "1"
PAGE   : "129-143"
YEAR   : "1976-00"
DOI    : "10.1029/SP007p0129"
TOPKEY : "solar activity"

---
MARKER : "1975_solar_phys_41_415"
TYPE   : "in_journal"
AUTHOR : "Feiter, L.D., Svestka, Z."
TITLE  : "On the behaviour of the hydrogen Lyman series in flares"
SERIAL : "Solar Phys."
VOLUME : "41 (2)"
PAGE   : "415-424"
YEAR   : "1975-04"
DOI    : "10.1007/BF00154078"
TOPKEY : "flares"
ABS    : "The Lyman spectrum of hydrogen has been computed for a number of flare models, characterized by the column density of hydrogen atoms in the ground state (N_1), the electron density (n_e) and the electron temperature (T_e). Broadening by the thermal Doppler effect and by Stark effect has been accounted for. The source functions for the individual lines of the series have been derived from non-LTE calculations of the excitation in hydrogen flares. The aim of the investigation is to evaluate the use of the intensities in between two successive Lyman lines for a determination of the value for N_1, which is a physical parameter of the flare for which only indirect determinations are available. Whilst in principle this method could givereliable results, its practical application meets with difficulties which hardly can be overcome. Therefore, one probably has to base the N1 determination on the highest line resolvable in the spectrum."

---
MARKER : "1975_assl_49"
TYPE   : "in_proceedings"
AUTHOR : "Dodson, N.W., Hedeman, E.R., Kreplin, R.W., Martres, M.J., Obridko, V.N., Shea, M.A., Smart, D.F., Tanaka, H., Svestka, Z., Simon, P."
TITLE  : "Catalog of solar particle events 1955-1969"
EDITOR : "Svestka, Z., Simon, P."
SERIAL : "Astrophysics and Space Science Library"
VOLUME : "49"
PAGE   : "(438 pages)"
YEAR   : "1975-06"
PUBLISH: "D. Reidel Publ. Co., Dordrecht"
TOPKEY : "solar particle events"
URL    : "http://www.springer.com/astronomy/astrophysics+and+astroparticles/book/978-90-277-0490-0"

---
MARKER : "1975_iau_symp_68_427"
TYPE   : "in_proceedings"
AUTHOR : "Svestka, Z."
TITLE  : "On the acceleration processes in solar flares"
CTITLE : "Proc. IAU Symp. 68 on Solar gamma-, X-, and EUV radiation"
PLACE  : "Buenos Aires, Argentina, 11-14 June 1974"
PAGE   : "427-439"
YEAR   : "1975-00"
DOI    : "10.1007/978-94-010-1802-9_39"
URL    : "http://adsabs.harvard.edu/abs/1975IAUS...68..427S"
TOPKEY : "flares"
ABS    : "The paper summarizes what we know about the acceleration processes on the Sun. Four different instabilities are distinguished: (1) One with purely thermal consequences giving rise to the origin of any flare. (2) A non-thermal process at the flash phase of flares giving rise to ~100 keV electrons and protons, manifested through hard X-ray and impulsive microwave bursts (current interruption?). (3) An instability giving rise to streams of electrons, without accelerating protons, manifested by type III bursts (tearing-mode instability?). When (2) and (3) are linked, flare associated electron events in space are often recorded. (4) Finally an explosive instability produces a shock wave which manifests itself as a type II burst. This instability leads to a second-step acceleration of particles preaccelerated in (2) and gives origin to &gt;10 MeV protons and relativistic electrons (probably stochastic acceleration)."

---
MARKER : "1974_solar_phys_36_417"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z., Fritzova-Svestkova, L."
TITLE  : "Type II radio bursts and particle acceleration"
SERIAL : "Solar Phys."
VOLUME : "36 (2)"
PAGE   : "417-431"
YEAR   : "1974-06"
DOI    : "10.1007/BF00151211"
TOPKEY : "radio bursts"
ABS    : "328 particle events recorded during 30 months from January 1, 1966 to June 30, 1968 (taken from the new Catalog of Solar Particle Events, 1955-1969) are compared with the occurrence of 166 type lI radio bursts during the same period. The results of this comparison give a convincing evidence that proton acceleration to higher energies in flares (the 'second acceleration step') is closely connected with the type II burst occurrence. The shock wave appears to originate near the time when the impulsive burst occurs, and the second acceleration step follows ]mmediately the first one; in some cases the second step sets in while the first step is still in progress. A detailed analysis indicates that we may need even three different acceleration mechanisms in flares: The first one gives rise to electrons which produce the microwave and hard X-ray bursts (and it probably also accelerates protons to low energies); the second, which sometimes coincides (but mostly does not coincide) with the first one, produces beams of electrons which give rise to type III bursts; and the third one, characterized by the type 1I burst-producing shock wave, accelerates (on some, rather rare occasions) the particles, preaccelerated by the first mechanism, to higher energies."

---
MARKER : "1973_solar_phys_31_389"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "The H_alpha flare as a secondary product of a coronal instability"
SERIAL : "Solar Phys."
VOLUME : "31 (2)"
PAGE   : "389-400"
YEAR   : "1973-08"
DOI    : "10.1007/BF00152815"
TOPKEY : "flares"
ABS    : "The assumption that the flare originates in the corona or transition layer, is confronted with the known properties of chromospheric flares. It is concluded that the basic mode of the energy transport into chromosphere is heat conduction. Only in some flares non-thermal particles contribute to the brightening in lower atmospheric layers: electrons with energy close to 100 keV produce chromospheric bright patches, and protons above 20 MeV cause the photospheric enhancements. The particle-produced brightenings are superposed on the basic quasi-thermal flare and involve only small areas as compared with the extensive regions heated through conduction. The most probable height of the flare origin appears to be close to the transition layer, between some 4000 and 7000 km above the photosphere. The non-thermal acceleration (when present) occurs probably higher than where the flare originates. There is no obvious reason why the high electron density in chromospheric flares could not be explained as simply due to increased ionization in the existing plasma, without any flare-induced mass condensations.  Though there are several facts supporting the flare origin in the corona (or transition layer), one cannot exclude the alternative that the flare instability involves simultaneously a wide (and in different cases different) range of altitudes. Energy considerations give some support to such a supposition."

---
MARKER : "1973_solar_phys_29_417"
TYPE   : "in_journal"
AUTHOR : "Fritzova-Svestkova, L., Svestka, Z."
TITLE  : "A comment on the flare activity in August 1972"
SERIAL : "Solar Phys."
VOLUME : "29 (2)"
PAGE   : "417-419"
YEAR   : "1973-04"
DOI    : "10.1007/BF00150821"
TOPKEY : "flares"

---
MARKER : "1973_solar_terr_relations_23"
TYPE   : "in_proceedings"
AUTHOR : "Svestka, Z."
TITLE  : "Observational aspects of flares"
CTITLE : "Proc. on Solar Terrestrial Relations"
PLACE  : "Calgary, Canada, 28 August-1 September 1972"
PAGE   : "23"
YEAR   : "1973-00"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1973str..conf...23S"

---
MARKER : "1972_ann_rev_astron_astrophys_10_1"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Spectra of solar flares"
SERIAL : "Annual Review of Astronomy and Astrophysics"
VOLUME : "10"
PAGE   : "1-24"
YEAR   : "1972-09"
DOI    : "10.1146/annurev.aa.10.090172.000245"
TOPKEY : "flares"
ABS    : "Solar flares emit electromagnetic radiation within a very broad range of wavelengths, from 0.02 &Aring; (2&times;10<sup>-10</sup>) up to more than 600 m (6&times;10<sup>4</sup> cm). This may be continuous emission in some parts of the spectrum, line emission in other, or a combination of both. These different kinds of radiation, of course, come from different heights in the solar atmosphere and thus from different parts of the flare. This paper will discuss only the flare spectrum in the region accessible to the ground-baed toptical solar spectrographs, while other parts of the spectrum will be mentioned only if necessary for the understanding of the optical observations."

---
MARKER : "1972_space_sci_rev_13_824"
TYPE   : "in_proceedings"
AUTHOR : "Svestka, Z., de Feiter, L.D."
TITLE  : "The expected behaviour of the hydrogen Lyman lines in solar flares"
CTITLE : "Proc. 3^rd Symp. on Ultraviolet and X-ray spectroscopy of astrophysical and laboratory plasmas"
PLACE  : "Utrecht, Netherlands, 24-26 August 1971"
SERIAL : "Space Sci. Rev."
VOLUME : "13 (45-46)"
PAGE   : "824"
YEAR   : "1972-09"
DOI    : "10.1007/BF00213515"
TOPKEY : "flares"

---
MARKER : "1972_spen_1"
TYPE   : "in_proceedings"
AUTHOR : "Svestka, Z."
TITLE  : "Characteristics of strong particle sources of the Sun"
EDITOR : "Ulwick, J.C."
CTITLE : "Proc. COSPAR Symp. on Solar particle event of November 1969"
PAGE   : "1"
YEAR   : "1972-08"
PLACE  : "Boston College, Chestnut Hill, MA, 16-18 June 1971"
URL    : "http://adsabs.harvard.edu/abs/1972spen.conf....1S"

---
MARKER : "1972_solar_phys_25_3"
TYPE   : "in_journal"
AUTHOR : "de Jager, C., Svestka, Z."
TITLE  : "Editorial"
SERIAL : "Solar Phys."
VOLUME : "25 (1)"
PAGE   : "3-4"
YEAR   : "1972-07"
DOI    : "10.1007/BF00155739"
REMARK : "editorial"

---
MARKER : "1972_solar_phys_24_498"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Book review"
SERIAL : "Solar Phys."
VOLUME : "24 (2)"
PAGE   : "498"
YEAR   : "1972-06"
DOI    : "10.1007/BF00153391"
REMARK : "book review"

---
MARKER : "1972_solar_phys_24_154"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Spectral analysis of highly inhomogeneous chromospheric flares"
SERIAL : "Solar Phys."
VOLUME : "24 (1)"
PAGE   : "154-168"
YEAR   : "1972-05"
DOI    : "10.1007/BF00231093"
TOPKEY : "flares"

---
MARKER : "1972_assl_29_72"
TYPE   : "in_proceedings"
AUTHOR : "Svestka, Z."
TITLE  : "Solar discrete particle events"
EDITOR : "de Jager, C., Dyer, E.R."
CTITLE : "Proc. Intl Symp. on Solar-Terrestrial Physics, The sun: Part I of solar-terrestrial physics/1970"
PLACE  : "Leningrad, USSR, 12-19 May 1970"
SERIAL : "Astrophysics and Space Science Library"
VOLUME : "29"
PAGE   : "72-86"
YEAR   : "1972-00"
DOI    : "10.1007/978-94-010-3126-4_7"
PUBLISH: "Reidel, Dordrecht"
TOPKEY : "solar particle events"
ABS    : "The review paper discusses the following items in particular: Classification of particle events and the problem whether all flares are associated with particle emission of some kind; relations of the flare capability of particle emission to properties of associated active regions; differences in the size of proton events and the reasons for them; our improving knowledge of electron events, pure electron and proton events, and the possibility of two different acceleration processes on the sun; directly observed evidence of acceleration processes on the sun and some consequences deduced from these observations; the acceleration phase in the flare development."

---
MARKER : "1972_space_research_xii_1547"
TYPE   : "in_journal"
AUTHOR : "de Feiter, L.D., Svestka, Z."
TITLE  : "Neutron and gamma-ray emission from white-light flares"
SERIAL : "Space Research"
VOLUME : "XII (2)"
PAGE   : "1547-1551"
YEAR   : "1972-00"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1972spre.conf.1547D"

---
MARKER : "1972_progress_astronautics_30_141"
TYPE   : "in_proceedings"
AUTHOR : "Svestka, Z."
TITLE  : "Several solar aspects of flare-associated particle events"
EDITOR : "McIntosh, P.S., Dryer, M."
CTITLE : "Solar activity observations and predictions"
SERIAL : "Progress in Astronautics and Aeronautics"
VOLUME : "30"
PAGE   : "141"
YEAR   : "1972-00"
PUBLISH: "MIT Press"
TOPKEY : "flares, solar particle events"
URL    : "http://adsabs.harvard.edu/abs/1972PrAA...30..141S"

---
MARKER : "1971_solar_phys_21_3"
TYPE   : "in_journal"
AUTHOR : "de Jager, C., Švestka, Z."
TITLE  : "Editorial"
SERIAL : "Solar Phys."
VOLUME : "21 (1)"
PAGE   : "3"
YEAR   : "1971-12"
DOI    : "10.1007/BF00155766"
REMARK : "editorial"

---
MARKER : "1971_solar_phys_19_202"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "On the flux of neutrons from flares"
SERIAL : "Solar Phys."
VOLUME : "19 (1)"
PAGE   : "202-206"
YEAR   : "1971-08"
DOI    : "10.1007/BF00148834"

---
MARKER : "1971_phil_trans_royal_soc_london_270_157"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Solar particle events"
SERIAL : "Phil. Trans. Royal Soc. London A (Mathematical and Physical Sciences)"
VOLUME : "270 (1202)"
PAGE   : "157-165"
YEAR   : "1971-07"
DOI    : "10.1098/rsta.1971.0070"

---
MARKER : "1971_solar_phys_17_287"
TYPE   : "in_journal"
AUTHOR : "de Jager, C., Svestka, Z."
TITLE  : "Editorial"
SERIAL : "Solar Phys."
VOLUME : "17 (2)"
PAGE   : "287"
YEAR   : "1971-04"
DOI    : "10.1007/BF00150032"
REMARK : "editorial"

---
MARKER : "1971_solar_phys_17_212"
TYPE   : "in_journal"
AUTHOR : "Fritzova-Svestkova, L., Svestka, Z."
TITLE  : "Longitudinal distribution of PCA sources on the sun"
SERIAL : "Solar Phys."
VOLUME : "17 (1)"
PAGE   : "212-217"
YEAR   : "1971-03"
DOI    : "10.1007/BF00152873"
TOPKEY : "flares"
 
---
MARKER : "1971_cesra_1_15"
TYPE   : "in_proceedings"
AUTHOR : "Svestka, Z."
TITLE  : "Solar radio astronomy from the optical solar researchers point of view"
EDITOR : "Fokker, A."
CTITLE : "Proc. CESRA-1, 18-19 February 1971, Utrecht, Netherlands"
PAGE   : "15-30"
YEAR   : "1971-00"
URL    : "http://adsabs.harvard.edu/abs/1971cesra...1...15S"
TOPKEY : "solar physics"

---
MARKER : "1970_solar_phys_13_471"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "The phase of particle acceleration in the flare development"
SERIAL : "Solar Phys."
VOLUME : "13 (2)"
PAGE   : "471-489"
YEAR   : "1970-08"
DOI    : "10.1007/BF00153567"
TOPKEY : "flares"

---
MARKER : "1970_solar_phys_12_332"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Solar research at the Ondrejov Observatory"
SERIAL : "Solar Phys."
VOLUME : "12 (2)"
PAGE   : "332-340"
YEAR   : "1970-05"
DOI    : "10.1007/BF00227126"
TOPKEY : "solar physics"

---
MARKER : "1970_solar_phys_12_502"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Book reviews"
SERIAL : "Solar Phys."
VOLUME : "12 (3)"
PAGE   : "502-503"
YEAR   : "1970-06"
DOI    : "10.1007/BF00148031"
REMARK : "book review"

---
MARKER : "1970_assl_19_90"
TYPE   : "in_proceedings"
AUTHOR : "Svestka, Z."
TITLE  : "Particle event forecasting"
EDITOR : "Manno, V., Page, D.E."
CTITLE : "Proc. 3^rd ESLAB/ESRIN Symp. on Intercorrelated satellite observations related to solar events"
PLACE  : "Noordwijk, Netherlands, 16-19 September 1969"
SERIAL : "Astrophys. Space Science Library"
VOLUME : "19"
PAGE   : "90-101"
YEAR   : "1970-00"
DOI    : "10.1007/978-94-010-3278-0_6"
PUBLISH: "Reidel, Dordrecht"
TOPKEY : "solar particle events"
ABS    : "The paper reviews the present state of the forecasting problem. The solar particle events are first classified according to the classification scheme proposed by Smart and Shea. Main characteristics of proton-active regions are then summarized: magnetically complex type of the region, increase of the magnetic-field gradient, &delta;-configuration and A-configuration of the sunspot group, intensification and hardening of the microwave and X-ray spectrum, increased activity in the X-ray and microwave spectral regions, permanent emission of ~1 MeV proton flux, and loop-prominence-system occurrence. Characteristic properties of proton flares in the H&alpha;-light, X-ray and radio spectrum also are mentioned, as well as the influence of the flare position on the solar disk on the particle flux recorded in the earth's surroundings. Basic principles of the long-term forecasts are explained in the last paragraph: active longitudes, complexes of activity, permanent proton flux, and travelling impulses of solar activity are mentioned."

---
MARKER : "1970_space_research_x_817"
TYPE   : "in_journal"
AUTHOR : "Krivsky, L., Svestka, Z"
TITLE  : "The solar proton flares of June and November 1968 and February 1969"
SERIAL : "Space Research"
VOLUME : "X"
PAGE   : "817-824"
YEAR   : "1970-00"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1970spre.conf..817K"

---
MARKER : "1970_space_research_x_797"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Solar particle events"
SERIAL : "Space Research"
VOLUME : "X"
PAGE   : "797-816"
YEAR   : "1970-00"
TOPKEY : "Solar particle events"
URL    : "http://esoads.eso.org/abs/1970spre.conf..797S"

---
MARKER : "1970_trans_iau_14a_71"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Solar activity"
SERIAL : "Trans. Int. Astron. Union (Reports on Astronomy)"
VOLUME : "14A"
PAGE   : "71-110"
YEAR   : "1970-00"
TOPKEY : "solar activity"
URL    : "http://adsabs.harvard.edu/abs/1970IAUTA..14...71S"
ABS    : "The reader is kindly asked to consider this report for some sort of greatly unbalance equilibrium between the pressure exercised by the steadily increasing flow of papers discussing the vastly extending subject of solar activity, and the equally steady pressure exercised by the editor who insists on havig this report twice as short as three years ago. Therefore, some selection of the subjects and papers had to be made, a fairly severe one, since only about one third of all published papers could have been mentioned in the references, and I am well aware that almost everyone who will read the report, could suggest some improvement of the selection scheme. Nevertheless, I believe that the report as it stands, can fulfill its basic purpose, i.e. to give to the readers a general picture on the progress, which has been achieved in the field of solar activity research since the Prague meeting and on some of the research activities which are in progress at the present time. It is a great pleasure to acknowledge the enormous help I have received from the authors of the individual sections of the Draft Report, as well as from many other members of the Commission, who have very kndly provided me, or the co-authors, with useful information on the recent progress of their work. It is necessary to add that some highly valuable comments made by V. Bumba, J.T. Jefferies, C. Sawyer, E. v. P. Smith, B. Valnicek and J.M. Wilcox, have also been included in other chapters than those prepared by themselves."

---
MARKER : "1969_solar_phys_10_243"
TYPE   : "editorial"
AUTHOR : "de Jager, C., Svestka, Z."
TITLE  : "Editorial"
SERIAL : "Solar Phys."
VOLUME : "10 (2)"
PAGE   : "243"
YEAR   : "1969-12"
DOI    : "10.1007/BF00145510"
TOPKEY : "editorial"

---
MARKER : "1969_solar_phys_10_3"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z., Simon, P."
TITLE  : "Proton Flare Project, 1966. Summary of the August/September particle events in the McMath Region 8461."
SERIAL : "Solar Phys."
VOLUME : "10 (1)"
PAGE   : "3-59"
YEAR   : "1969-11"
DOI    : "10.1007/BF00146153"
TOPKEY : "flares"
ABS    : "The paper summarizes observations of solar and space phenomena related to the McMath region Number 8461 which passed over the solar disk during the 1966 Proton Flare Project period, from August 21 to September 4, and produced two important solar particle events on August 28 and September 2. The most important results are reviewed and interpretation of some of them is suggested. Items of particular interest: Occurrence of proton-active regions when two or more 'rows' of activity approach each other (Section 3). Possible stimulation of activity by magnetic fields of decaying regions that had been active before (4.2a, 5.1a). Significantly increased correlation of flares with X-ray bursts during the proton-active transit of the region (5.3b). Striking difference in the flare response in radio frequency range before and after August 26 (5.2b). Hardening of the X-rays (5.3a), increase in radio flux (5.2a), change in sunspot configuration (5.1c), and increased capability of the region for particle acceleration (5.1b, 5.2b), starting about three days prior to the proton flare. Clear evidence that some flares that occurred on or after August 26, but prior to the proton flare of August 28, already were sources of ~1 MeV protons (5.2b, 8). Anomalous deficiency in metric component of radio bursts produced in the region (5.2c, 9.4d, 11.4b). Strong radio storm on meter waves immediately preceding the proton flare on August 28 (5.2a, 9.1b), coincident with preflare rising dark filament (9.1a) and slight preflare rise in flux of ~ 1 MeV protons (10.2). Two phases of expansion (fast and slow) of the bright flare ribbons (9.2c). Coincidence of hard X-ray burst with the formation and fast separation of the bright flare ribbons. It is suggested that this is the time of particle acceleration in the flare (9.5b). Short-lived burst of UV radiation (9.6). Visible flare wave in the flare of August 28 (9.3b), and complexity of motions in this flare (9.4b). Suggested electron release by means of a blast wave (10.1a). Electron-proton splitting in the delayed shock-wave-associated maximum of the particle flux on August 29 (10.2c). First brightening of both proton flares in a similar position between the regions 8461 and 8459 (11.2c). Existence of a unique, low elevation coronal condensation three days after proton flare occurrences (7.2). Very strong flux of protons in energy range of the order of 100 MeV producing the largest PCA since July 1961, and unusually steep energy spectrum above 100 MeV in the flare of September 2 (12.2a, b, 12.4). Unusually long rise to the maximum flux, inconsistent with Burlaga's theory of anisotropic diffusion (12.2b). Interpretation of the undisturbed flux decay from September 2 to September 8 (12.2c). A corotating modulation phenomenon on September 8 (12.2d). Detection of medium nuclei, with He/M ratio 50&plusmn;11 (12.3a). Evidence against a purely velocity-dependent mode of particle propagation (12.3b). Electrons as the possible cause of the first PCA phase (12.4). Plasma disturbance due to permanent proton flux from the region (13.1). Electron injection into inner radiation belt during the geomagnetic storm associated with the September 2 flare (13.3). Section 14 brings a time scheme of the most important phenomena associated with the complex of activity and the active region in question, and some unsolved problems of particular interest are pointed out in Section 15."

---
MARKER : "1969_solar_phys_8_400"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Comment on the note by Friedman and Hamberger"
SERIAL : "Solar Phys."
VOLUME : "8 (2)"
PAGE   : "400"
YEAR   : "1969-08"
DOI    : "10.1007/BF00155387"
TOPKEY : "flares"
REMARK : "research note"

---
MARKER : "1969_solar_phys_8_3"
TYPE   : "editorial"
AUTHOR : "Svestka, Z., de Jager, C."
TITLE  : "Editorial"
SERIAL : "Solar Phys."
VOLUME : "8 (1)"
PAGE   : "3-4"
YEAR   : "1969-07"
DOI    : "10.1007/BF00150650"
TOPKEY : "editorial"

---
MARKER : "1969_solar_phys_6_155"
TYPE   : "in_journal"
AUTHOR : "Pasachoff, J.M., Gussmann, E.A., Stepanyan, N.N., Feiter, L.D., Uchida, Y., al., et"
TITLE  : "Abstracts of papers from other journals"
SERIAL : "Solar Phys."
VOLUME : "6 (1)"
PAGE   : "155-164"
YEAR   : "1969-01"
DOI    : "10.1007/BF00146806"
TOPKEY : "solar physics"

---
MARKER : "1969_ann_iqsy_3_469"
TYPE   : "in_journal"
AUTHOR : "Simon, P., Svestka, Z."
TITLE  : "General summary on the results of the first Proton Flare Project Period, July 1966"
SERIAL : "Ann. IQSY"
VOLUME : "3"
PAGE   : "469-500"
YEAR   : "1969-00"
TOPKEY : "flares"

---
MARKER : "1969_symp_csr_11"
TYPE   : "proceedings"
EDITOR : "de Jager, C., Svestka, Z."
TITLE  : "Proc. COSPAR Symp. on Solar flares and space research"
PLACE  : "11^th Plenary Meeting of the Committee on Space Research, Tokyo, Japan, May 9-11, 1968"
PUBLISH: "North-Holland Publ. Co., Amsterdam"
YEAR   : "1969-00"
TOPKEY : "flares"

---
MARKER : "1969_symp_csr_11_16"
TYPE   : "in_proceedings"
AUTHOR : "Svestka, Z."
TITLE  : "The optical flare"
CTITLE : "Proc. COSPAR Symp. on Solar flares and space research"
PLACE  : "11^th Plenary Meeting of the Committee on Space Research, Tokyo, Japan, May 9-11, 1968"
PAGE   : "16"
YEAR   : "1969-00"
TOPKEY : "flares"
PUBLISH: "North-Holland Publ. Co., Amsterdam"

---
MARKER : "1969_symp_csr_11_319"
TYPE   : "in_proceedings"
AUTHOR : "Svestka, Z."
TITLE  : "Effects associated with the sector boundary crossing on 8 July 1966"
CTITLE : "Proc. COSPAR Symp. on Solar flares and space research"
PLACE  : "11^th Plenary Meeting of the Committee on Space Research, Tokyo, Japan, May 9-11, 1968"
PAGE   : "319"
YEAR   : "1969-00"
TOPKEY : "sector boundary"
PUBLISH: "North-Holland Publ. Co., Amsterdam"

---
MARKER : "1968_iau_symp_35_287"
TYPE   : "in_proceedings"
TITLE  : "Loop-prominence systems and proton-flare active regions"
AUTHOR : "Svestka, Z."
EDITOR : "Kiepenheuer, K.O."
CTITLE : "IAU Symp. No. 35, Structure and development of solar active regions"
PAGE   : "287"
YEAR   : "1968-00"
TOPKEY : "flares"
PUBLISH: "Reidel, Dordrecht"
URL    : "http://adsabs.harvard.edu/abs/1968IAUS...35..287S"

---
MARKER : "1968_iau_symp_35_513"
TYPE   : "in_proceedings"
TITLE  : "Proton Flare Project, introduction and summary"
AUTHOR : "Svestka, Z."
EDITOR : "Kiepenheuer, K.O."
CTITLE : "IAU Symp. No. 35, Structure and development of solar active regions"
PAGE   : "513"
YEAR   : "1968-00"
TOPKEY : "flares"
PUBLISH: "Reidel, Dordrecht"
URL    : "http://adsabs.harvard.edu/abs/1968IAUS...35..513S"

---
MARKER : "1968_nobel_symp_9_17"
TYPE   : "in_proceedings"
AUTHOR : "Svestka, Z."
TITLE  : "Mass motions in flares indicated by line profiles and filtergrams"
EDITOR : "Oehman, Y."
CTITLE : "Proc. 9^th Nobel Symp. on Mass motions in solar flares and related phenomena"
PLACE  : "Anacapri, Italy, 10-12 June 1968"
PAGE   : "17"
YEAR   : "1968-00"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1968mmsf.conf...17S"

---
MARKER : "1968_solar_phys_5_259"
TYPE   : "in_journal"
AUTHOR : "de Jager, C., Svestka, Z."
TITLE  : "Editorial"
SERIAL : "Solar Phys."
VOLUME : "5 (3)"
PAGE   : "259"
YEAR   : "1968-11"
DOI    : "10.1007/BF00147139"
TOPKEY : "editorial"

---
MARKER : "1968_solar_phys_4_361"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Effects associated with the sector boundary crossing on July 8, 1966"
SERIAL : "Solar Phys."
VOLUME : "4 (3)"
PAGE   : "361-372"
YEAR   : "1968-07"
DOI    : "10.1007/BF00149567"
TOPKEY : "sector boundary"
ABS    : "Satellite measurements have shown that in such a case &lt;20 MeV protons are stored within the range of the sector boundary and with decreasing energy the particles tend to accumulate towards and behind the Eastern boundary limit; low-energy particles, such as &lt;50 keV electrons, are stored exclusively behind this Eastern limit. The boundary crossing caused a short-lived geomagnetic disturbance, a PCA enhancement in lower latitudes, a two-phase ionospheric disturbance, and a transient cosmic-ray decrease on neutron monitors looking westward immediately after the sector boundary passed the earth. The storage of low-energy particles on the Eastern side of the boundary may indicate a preference of the transverse diffusion for the Westward direction in interplanetary space."

---
MARKER : "1968_solar_phys_4_18"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "On long-term forecasts of proton flares"
SERIAL : "Solar Phys."
VOLUME : "4 (1)"
PAGE   : "18-29"
YEAR   : "1968-05"
DOI    : "10.1007/BF00146995"
TOPKEY : "flares"
ABS    : "174 proton flares which were observed during the period from 1956 to 1965, occurred in 81 different active regions. It is shown that these active regions formed in complexes of activity, which stayed on the solar surface for many months, and in some cases even for several years. Since the proton-flare regions develop very rapidly and reach the proton-flare active stage within a few days, these complexes of activity represent the areas on the sun, where proton-flare regions can form at any time. Reference is made to contributions by Bumba and Howard, who investigated the birth of active regions and detected some properties of complexes of activity; nevertheless, at the present time, we do not know any method to predict when a proton-flare region begins to develop in such a complex of activity. On the other hand, there is a chance of predicting the dangerous longitudes on the sun, as soon as such a complex of activity has been well recognized or, from the opposite point of view, to predict the safe proton-flare free periods on the sun. If, however, all the complexes on both the hemispheres are taken into account and every complex is considered 'proton-dangerous' from 2 days before to 7 days after the central meridian passage, one can prove that no proton-flare free periods existed for more than 3 years around the maximum of the last solar cycle. Applying this result to the present cycle, one can conclude that no safe forecasts of proton-flare free periods can be made from the beginning of 1968 to the end of 1970. During the remaining 7 or 8 years of the solar cycle, long-term forecasts of proton flares could be made provided that our knowledge of the formation and development of the complexes of activity is improved. It is of interest to notice some properties of the complexes formed in the last solar cycle. While the complexes on the Northern solar hemisphere remained at fairly constant heliographic longitudes for many years, the complexes formed on the Southern hemisphere seemed to travel in two rows around the sun, in the direction opposite to the solar rotation. Another interesting fact is a yearly periodicity in the formation of proton-flare regions in the complexes of activity, with a maximum in the summer period and a deep minimum in the winter season. Such a seasonal variation also appears, if one considers the flare activity, type-IV bursts, PCA's, great magnetic storms, and magnetic crochets. Therefore, one can reasonably believe that this yearly variation, even when similar to the seasonal variation at the earth, is of solar origin."

---
MARKER : "1968_solar_phys_3_3"
TYPE   : "in_journal"
AUTHOR : "de Jager, C., Svestka, Z."
TITLE  : "Editorial"
SERIAL : "Solar Phys."
VOLUME : "3 (1)"
PAGE   : "3"
YEAR   : "1968-01"
DOI    : "10.1007/BF00154236"
TOPKEY : "editorial"

---
MARKER : "1967_solar_phys_2_75"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z., Fritzova-Svestkova, L."
TITLE  : "Electron density in flares I: Discussion of the halfwidth method"
SERIAL : "Solar Phys."
VOLUME : "2 (1)"
PAGE   : "75-86"
YEAR   : "1967-07"
DOI    : "10.1007/BF00155893"
TOPKEY : "flares"
ABS    : "The halfwidth method used for the determination of the electron density in flares is discussed from the point of view of possible errors which may enter the obtained results. The discussion includes an analysis of errors of measurement as well as errors of the method due to: (1) our incomplete knowledge of the electron damping, (2) the assumption of constant electron temperature, (3) the presence of residual self-absorption in high Balmer lines, and (4) possibly present non-thermal motions. It is shown that the factors (2) to (4) cannot induce any relative error in ne higher than 30% of the correct value, and the actual error usually is smaller. A comparison is made of the halfwidth-method application to active prominences and limb flares."

---
MARKER : "1967_solar_phys_2_87"
TYPE   : "in_journal"
AUTHOR : "Fritzova-Svestkova, L., Svestka, Z."
TITLE  : "Electron density in flares II: Results of measurements"
SERIAL : "Solar Phys."
VOLUME : "2 (1)"
PAGE   : "87-97"
YEAR   : "1967-07"
DOI    : "10.1007/BF00155894"
TOPKEY : "flares"
ABS    : "Measurements of the electron density in 16 flares are summarized and discussed. For 13 of them the electron density has been determined by the halfwidth method discussed in Part I of this paper. In the flash phase of all disk flares of importance 1+ and higher the electron density exceeds 10<sup>13</sup> cm<sup>-3</sup> and increases with the flare importance. In the maximum of large flares the electron density exceeds 3&times;10<sup>13</sup> cm<sup>-3</sup> and declines to 10<sup>13</sup> cm<sup>-8</sup> and to lower values in about 20 minutes after the flash phase. In limb flares, i.e. higher than 5000 km above the solar limb, the electron density is lower than 5&times;10<sup>12</sup> cm<sup>-3</sup>. This shows a decrease of the electron density in the flare elements situated in higher parts of the chromosphere. On the other hand, however, at least in some flares the electron density remains fairly constant within a wide range of height in the upper chromosphere and the low corona.
"

---
MARKER : "1967_solar_phys_1_303"
TYPE   : "in_journal"
AUTHOR : "de Jager, C., Svestka, Z."
TITLE  : "editorial"
SERIAL : "Solar Phys."
VOLUME : "1 (3-4)"
PAGE   : "303"
YEAR   : "1967-06"
DOI    : "10.1007/BF00151358"
TOPKEY : "editorial"

---
MARKER : "1967_solar_phys_1_3"
TYPE   : "in_journal"
AUTHOR : "de Jager, C., Svestka, Z."
TITLE  : "Editorial (first Solar Physics Issue)"
SERIAL : "Solar Phys."
VOLUME : "1 (1)"
PAGE   : "3-4"
YEAR   : "1967-01"
DOI    : "10.1007/BF00150299"
TOPKEY : "editorial"

---
MARKER : "1967_baic_18_55"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Type IV bursts. III. In association with Forbush effects"
SERIAL : "Bull. Astron. Inst. Czech."
VOLUME : "18"
PAGE   : "55"
YEAR   : "1967-00"
TOPKEY : "flares"
REMARK : "received 23 Aug 1966"
URL    : "http://adsabs.harvard.edu/abs/1967BAICz..18...55S"
ABS    : "Eighty-five Forbush decreases associated with type IV burst flares listed in Paper I are discussed, particularly in relation to the PCA events investigated in Paper II. The three main conclusions of this discussion can be summarized as follows: 1. The productivity of Forbush effects by type IV burst flares strongly increases with the increasing importance of the associated PCA event. This proves that the space density of high-energey particles can only be high if the total density of particles inside the cloud is high. 2. The delay times of GLE's, PCA's and Forbush decreases show one common characteristic: If the effect is strong, the delay time is always short. A short delay time itself, however, does not mean that the effect is strong. An explanation of this characteristic feature is given. 3. While there are very few flares producing strong PCA's to the east of the solar central meridian and the vast majority of strong PCA events is caused by flares situated on the western solar hemisphere, the majority of flares producing major cosmic-ray storms are on the eastern hemisphere of the Sun. Flares nearer to the western limb than 50&deg;W, very efficient in producing strong PCA's, are entirely inactive in producing major cosmic-ray storms. It is shown that one can explain this longitude distribution of flares producing Forbush effects and/or PCA's when assuming an asymmetrical distribution of the magnetic field inside the cloud of the ejected particles, with a strong magnetic western boundary of the cloud."

---
MARKER : "1966_baic_17_4"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z., Olmr, J."
TITLE  : "Type IV bursts, I: List of events"
SERIAL : "Bull. Astron. Inst. Czech."
VOLUME : "17 (1)"
PAGE   : "4-16"
YEAR   : "1966-00"
TOPKEY : "flares"
REMARK : "12 May 1965"
URL    : "http://adsabs.harvard.edu/abs/1966BAICz..17....4S"
ABS    : "A list of 174 type IV events recorded during 1956-1963 is given. This catalogue is based on Sydney, Harvard and Boulder dynamic spectra, single frequency summaries published in the Quarterly Bulletin on Solar Activity and single frequency records at Ondrejov. One can estimate that about 75% of all type IV bursts which occurred on the Sun during the Years 1956-1963 are included in the catalogue."

---
MARKER : "1966_baic_17_95"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "A prediction on proton flare occurrence in 1966-1968"
SERIAL : "Bull. Astron. Inst. Czech."
VOLUME : "17"
PAGE   : "95"
YEAR   : "1966-00"
TOPKEY : "flares"
REMARK : "received 22 Feb 1966"
URL    : "http://adsabs.harvard.edu/abs/1966BAICz..17...95S"
ABS    : "abstract in Czech"

---
MARKER : "1966_baic_17_137"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "The H^_ emission in flares"
SERIAL : "Bull. Astron. Inst. Czech."
VOLUME : "17 (3)"
PAGE   : "137-140"
YEAR   : "1966-00"
TOPKEY : "flares"
REMARK : "received 8 Dec 1965"
URL    : "http://adsabs.harvard.edu/abs/1966BAICz..17..137S"
ABS    : "Since all processes discussed hitherto have failed to explain the continuous emission of flares in the optical region, it is of interest to note that the formation of negative hydrogen ions in flares cannot be fully rejected as the possible cause of the flare continua. Using known physical data on three solar flares, it is shown that this process could produce the observed continuous emission in such flares or flare elements, in which the Lyman alpha radiation temperature is lower than ~7500&deg;K. If such flares or flare elements existed, they would probably be situated very low in the chromosphere. In such a case, a heating of the upper photospheric layers beneath the flare or of some grains inside the photosphere might also participate in the formation of the flare continua. The wavelength variation of the relative intensity of the H<sup>;&plusmn;</sup> continuous emission is in good agreement with observation for flares situated in limb parts of the solar disc."

---
MARKER : "1966_baic_17_249"
TYPE   : "in_journal"
AUTHOR : "Fritzova, L., Svestka, Z."
TITLE  : "Type IV bursts, II: In association with PCA events"
SERIAL : "Bull. Astron. Inst. Czech."
VOLUME : "17 (5)"
PAGE   : "249-261"
YEAR   : "1966-03"
TOPKEY : "flares"
REMARK : "received 20 Mar 1966"
URL    : "http://adsabs.harvard.edu/abs/1966BAICz..17..249F"
ABS    : "The new catalogues of 177 type IV bursts recorded during 1956-1963 (Paper I) in combination with a newly compiled list of 124 PCA's during that period has made it possible to investigate 81 events of type IV bursts associated with injections of high-energy protons into the polar ionosphere. A newly introduced classification of PCA importance, together with the extended number of correctly associated events, leads to some new, improved, or verified results concerning PCA productions by proton flares occurring on the Sun. Seasonal variation of the PCA occurrence and delay time, western preference for flares producing strong PCA events and an absence of this preference for flares causing weak PCA's, a dependence of the delay time on the PCA importance, and a general tendency of some active regions to emit or not to emit high-energy protons from type IV burst flares to the Earth, are amongst the conclusions which are summarized in section 9."

---
MARKER : "1966_space_sci_rev_5_388"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Optical observations of solar flares"
SERIAL : "Space Sci. Rev."
VOLUME : "5 (3)"
PAGE   : "388-418"
YEAR   : "1966-05"
DOI    : "10.1007/BF02653250"
TOPKEY : "flares"
ABS    : "This paper gives a review of the results of optical observations of solar flares. Observations carried out in the H&alpha; line, flare spectra, and the methods of analysing the flare spectra are briefly discussed. Great attention is paid to the continuous emission of flares in the optical spectral region. In the last section, optical aspects of proton flares are summarized."

---
MARKER : "1966_baic_17_262"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Proton flares before 1956"
SERIAL : "Bull. Astron. Inst. Czechoslov."
VOLUME : "17 (5)"
PAGE   : "262-270"
YEAR   : "1966-03"
TOPKEY : "flares"
REMARK : "received 30 Mar 1966"
URL    : "http://adsabs.harvard.edu/abs/1966BAICz..17..262S"
ABS    : "Observational results of vertical incidence ionospheric soundings made at high latitude stations before 1956, made it possible to find 47 highly probable PCA events during 1938-1955 and to identify 32 of them with observed or hypothetical proton flares (these being unobserved flares in the only important active region on the solar disk present on the day of the PCA occurrence). These quite new PCA data fully confirm the deficiency of the PCA occurrence in the northern winter months, the very strong western preference for flares producing strong PCA events with a steep limit of occurrence at about 10&deg;E on the solar disk, the north-south asymmetry of flares producing PCA's, and the dependence of the PCA delay time on the season, PCA importance and heliographic longitude of the proton flare. A comparison of the records by vertical incidence soundings during 1956-1959 with known PCA data has allowed a fairly homogeneous set of data on strong PCA's to be obtained for the whole period 1938-1963 and some conclusions to be drawn on the PCA occurrence in various phases of the solar activity. A relative decrease of the number of obsered PCA events during the maximum phase of the solar cycle is in a good agreement with the well-known absence of GLE's in the maximum years. It can be predicted that about 10 PCA's can be expected in 1966 and yearly about 25 events in 1967 and 1968, approximately 30% of them being strong PCA events."

---
MARKER : "1965_adv_astron_astrophys_3_119"
TYPE   : "in_journal"
AUTHOR : "Švestka, Z."
TITLE  : "title unknown"
SERIAL : "Adv. Astron. Astrophys."
VOLUME : "3"
PAGE   : "119"
YEAR   : "1965-00"

---
MARKER : "1964_baic_15_162"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Broadening of high Balmer lines in flares and prominences"
SERIAL : "Bull. Astron. Inst. Czech."
VOLUME : "15"
PAGE   : "162-163"
YEAR   : "1964-01"
REMARK : "received 8 Jan 1964"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1964BAICz..15..162S"
ABS    : "abstract in Czech"

---
MARKER : "1964_baic_15_117"
TYPE   : "in_journal"
AUTHOR : "de Feiter, L.D., Svestka, Z."
TITLE  : "Time variation of electron density in a large solar flare"
SERIAL : "Bull. Astron. Inst. Czech."
VOLUME : "15 (3)"
PAGE   : "117-118"
YEAR   : "1964-01"
REMARK : "received 5 Jan 1964"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1964BAICz..15..117D"
ABS    : "abstract in Czech"

---
MARKER : "1964_baic_15_38"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Electron temperature and b_n values in flares"
SERIAL : "Bull. Astron. Inst. Czech."
VOLUME : "15 (2)"
PAGE   : "38-41"
YEAR   : "1964-00"
URL    : "http://adsabs.harvard.edu/abs/1964BAICz..15...38S"
REMARK : "received 5 May 1963"
TOPKEY : "flares"
ABS    : "The method of determining T_e as a limit of excitation temperature T_^alpah;(s -> r) for increasing quantum numbers s and r, applied to the flares of August 7, 1960 and July 30, 1958, is verified and it is shown that it can be applied as long as the condition (9) is fulfilled. This seems to be the case in interior parts of the flares. On the other hand, in surface layers of flares the deviations from thermodynamic equilibrium are more pronounced and the method is not successful. The Balmer decrement is also used to estimate the relative values of b_n factors in the flares discussed (Table 2). With n_e=3 or 6&times;10^13 cm^-3 for the flare of August 7, 1960, the concentration of two-quantum atoms n_2 is found of the order of 10^9 cm^-3, which leads to a fictive geometrical thickness z of several or several tens of kilometers (Table 3). Thus the method applied presents further evidence of the filamentary structure of flares suspected earlier by Suemoto et al. (1962) and by the present writer (Svestka 1963)."

---
MARKER : "1963_baic_14_234"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Spectral analysis of the moustache-like flare of August 7, 1960"
SERIAL : "Bull. Astron. Inst. Czech."
VOLUME : "14 (6)"
PAGE   : "234-244"
YEAR   : "1963-02"
URL    : "http://adsabs.harvard.edu/abs/1963BAICz..14..234S"
TOPKEY : "flares"
REMARK : "received 14 Feb 1963"
ABS    : "The spectrum of the anomalous flare of August 7, 1960, situated close to the eastern solar limb, is studied in detail. A striking central absorption in the Balmer lines up to the H_8, the anomaly of the metal line intensities in the spectrum and an extraordinary X-ray emission recorded by the SR-1 satellite ouside the Earth's atmosphere are the peculiar characteristics of this interesting flare. Using the half-widths of high Balmer lines on finds n_e=6&times;10^13 cm^-3 and n_2.z=2.5&times;10^15 cm^-2 in the flare layer. Assuming Stark broadening of all the Balmer lines, T_e results lower than 10^4&deg;K. With these values, however, the Balmer continuum should be observed, if only the geometrical thickness z exceeds 5 kms. As no traces of any continuous emission were found behind the Balmer limit, we conclude that the flare had a filamentary structure consisting of highly excited flare filaments embedded in much less excited interflare matter. We believe that this is a general property of flares; of course, as a result many methods applied to the spectral analysis of flares in the past have yielded quite a false picture of the physical state in these active phenomena. The extremely strong absorption in the cores of Balmer lines as well as the anomalous behaviour of metal lines were due to the increased absorption above the flare along the line-of-sight. One can suppose that the density of chromospheric and coronal gas above the active region was increased by a factor 3 or 4 in two days or more, which could produce both the spectral anomalies observed as well as the extraordinary X-ray emission enhancements recorded at flares which appeared in that region on August 6 and 7, 1960."

---
MARKER : "1963_baic_14_146"
TYPE   : "in_journal"
AUTHOR : "Kopecky, M., Letfus, V., Blaha, M., Svestka, Z."
TITLE  : "Qualitative discussion of 244 flare spectra. IV. Splitting of metal emission lines"
SERIAL : "Bull. Astron. Inst. Czech."
VOLUME : "14 (4)"
PAGE   : "146-150"
YEAR   : "1963-00"
URL    : "http://adsabs.harvard.edu/abs/1963BAICz..14..146K"
TOPKEY : "flares"
REMARK : "received 1962-10"
ABS    : "It is shown that the splitting of some metal emission lines discovvered in the spectra of several flares over sunspots cannot be due to the Zeeman effect, because the Zeeman patterns of some split lines contradict this supposition. A discussion of the curve of growth of Fe I, however, shows that self-reversal of optically the thickest lines is the probable cause of their splitting. Assuming an absorbing layer over the flare as the cause of the self-reversal observed, the curve of growth allows its excitation temperature to be estimated at 4300&deg;-5000&deg;."

---
MARKER : "1963_baic_14_75"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "On the spectral analysis of flares"
SERIAL : "Bull. Astron. Inst. Czech."
VOLUME : "14 (3)"
PAGE   : "75-77"
YEAR   : "1963-00"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1963BAICz..14...75S"
ABS    : "A two-hour introductory lecture, presented here in an abstract only. Its main points will be published in two papers prepared for publication in the next numbers of BAC"

---
MARKER : "1963_orbit_dict"
TYPE   : "book"
AUTHOR : "Kleczek, J., Svestka, Z."
TITLE  : "Astronomicky a astronauticky slovnik"
YEAR   : "1963-00"
TOPKEY : "astronomy"
PUBLISH: "Orbis, Praha"

---
MARKER : "1962_baic_13_236"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Evidence of Stark broadening of Balmer lines in flares"
SERIAL : "Bull. Astron. Inst. Czech."
VOLUME : "13 (6)"
PAGE   : "236-240"
YEAR   : "1962-05"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1962BAICz..13..236S"
ABS    : "Using the measurement of half-widths of higher Balmer lines, evidence is given that Balmer lines in at least some flares (if not in all of them) are broadened by the Stark effect. If the Doppler broadening were effective in lower lines, it would have to confined to upper parts of the flare, optically thin and practically invisible for n&ge;8. Half-width measurement of Balmer lines in the moustache-like flare of August 7, 1960, proves that flares are not conglomerates of moustaches; moustaches and flares are evidently phenomena of a substantially different nature."

---
MARKER : "1962_baic_13_190"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Motions in chromospheric flares"
SERIAL : "Bull. Astron. Inst. Czech."
VOLUME : "13 (5)"
PAGE   : "190-198"
YEAR   : "1962-04"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1962BAICz..13..190S"
ABS    : "On the basis of a study of filtergrams some conclusions are drawn about the general properties of motions in chromospheric flares. Four main types of motion are distinguished: (1) Slow continuous ascent with velocities of 1-14 km/sec, flares dissipating high over the base of the chromosphere; (2) Fast ascent with maximum velocities in the limits of 30-140 km/sec, followed by a slower descent later on, probably the most frequent case of motion in flares; (3) High-speed ejections of parts of flares under various inclinations towards the solar surface, reaching distances up to 250,000 km, with velocities sometimes higher than 1000 km/sec; (4) Slow expansion of flares, which are formed by two parallel filaments and situated outside the regions of strong magnetic fields in sunspot groups. The expansion with velocities within the limits of 1-11 km/sec sometimes seems to be combined with a slow ascending motions described ad (1). This expansive motion does not appear if the two filaments of the flare are anchored inside a sunspot group, i.e. in regions with strong magnetic fields."

---
MARKER : "1962_baic_13_85"
TYPE   : "in_journal"
AUTHOR : "Blaha, M., Kopecky, M., Svestka, Z."
TITLE  : "Qualitative discussion of 244 flare spectra. III. Metal emission lines"
SERIAL : "Bull. Astron. Inst. Czech."
VOLUME : "13 (3)"
PAGE   : "85-91"
YEAR   : "1962-12"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1962BAICz..13...85B"
ABS    : "The third contribution to the qualitative discussion of 244 spectra of 92 chromospheric flares deals with the emission of metal lines in flare spectra. It examines the total intensity of the metal emission lines as related to other flare parameters (chiefly to the excitation of hydrogen lines), the V-effect, the variation in time of the intensity of these lines during the development of the flare, and their splitting. Discussed is the anticoincidence problem in the emission regions of hydrogen and metals. The results are summarized in Sec. 8."

---
MARKER : "1962_baic_13_37"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z., Kopecky, M., Blaha, M."
TITLE  : "Qualitative discussion of 244 flare spectra. II. Line assymmetry and helium lines"
SERIAL : "Bull. Astron. Inst. Czech."
VOLUME : "13 (2)"
PAGE   : "37-41"
YEAR   : "1962-07"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1962BAICz..13...37S"
ABS    : "The Paper presents the second part of a qualitative discussion of 244 spectra of 92 chromospheric flares. Attention is paid to the asymmetry of hydrogen and calcium lines and to some characteristics of the helium lines, &lambda;5875-8(D_3) and &lambda; 3964-7. The occurence of a red and blue asymmetry in flare spectra, centre-limb variation of the asymmetry, the occurrence of emission and absorption helium lines in flare spectra, centre-limb variation of the helium emission, and the connection between the helium emission and the line asymmetry are studied in detail. The conclusions drawn from this discussion are summarized in par.4."

---
MARKER : "1962_baic_13_35"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Note on planetary nebulae in the Small Magellanic Cloud"
SERIAL : "Bull. Astron. Inst. Czech."
VOLUME : "13 (1)"
PAGE   : "35-36"
YEAR   : "1962-07"
TOPKEY : "planetary nebulae"
URL    : "http://adsabs.harvard.edu/abs/1962BAICz..13...35S"

---
MARKER : "1962_baic_13_30"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "On a peculiar flare spectrum"
SERIAL : "Bull. Astron. Inst. Czech."
VOLUME : "13 (1)"
PAGE   : "30-33"
YEAR   : "1962-07"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1962BAICz..13...30S"
ABS    : "A peculiar flare spectrum characterized by a weak emission imbedded in an absorption is described and discussed. It is suggested that it originated in an approximately-spherical rotating ball with an emission core and an absorbing shell, which moved downwards through the chromosphere at a height of several thousand kilometres with a velocity of about 18 km/s. Spectral lines were broadened by microturbulent motions of characteristic velocity ~ 90 km/s."

---
MARKER : "1961_baic_12_229"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z., Kopecky, M., Blaha, M."
TITLE  : "Qualitative discussion of 244 flare spectra"
SERIAL : "Bull. Astron. Inst. Czech."
VOLUME : "12 (6)"
PAGE   : "229-237"
YEAR   : "1961-04"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1961BAICz..12..229S"
ABS    : "The Paper presents a list of flare emission lines observed in selected spectral regions in spectra of 92 flares photographed by the Ondrejov spectrograph during the years 1958-1960, and brings the first part of a qualitative discussion of 244 spectra of these flares, which concerns spectral characteristics of hydrogen and calcium lines: Variation of the Balmer series excitation with the H&alpha; central intensity and line-width; centre-limb variation of the Balmer series excitation, H&alpha; and H+K line-widths; dependence between the H&alpha; central intensity and line-width; dependence between H&alpha; and H+K line-widths; central reversal in hydrogen and calcium lines; variations of spectral characteristics as to the position of the flare region in sunspot groups; and the V-effect. The conclusions drawn from this discussion are summarized in par. 7."

---
MARKER : "1961_baic_12_47"
TYPE   : "in_journal"
AUTHOR : "Kvicala, F., Hrebik, F., Olmr, F., Svestka, Z., Krivsky, L."
TITLE  : "Observations of flares at the Ondrejov Observatory in the year 1959"
SERIAL : "Bull. Astron. Inst. Czech."
VOLUME : "12"
PAGE   : "47-70"
YEAR   : "1961-08"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1961BAICz..12...47K"
ABS    : "This paper is a continuation of five preceding reports, which contained flares observed at Ondrejov sinc 1948 up to the end of the I.G.Y. and covers the period of the I.G.C. It presents data about 479 flares, associated 808, 536, and 231 Mc/s events and 27 Kc/s enhancements of atmospherics observed and recorded during the year 1959. Figures contain curves of the H&alpha; line-width changes, selected radio events, effects of the S.E.A. on atmospheric, and some examples of flare spectra."

---
MARKER : "1961_baic_12_73"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Spectrum of the flare of July 20, 1958"
SERIAL : "Bull. Astron. Inst. Czech."
VOLUME : "12"
PAGE   : "73-81"
YEAR   : "1961-08"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1961BAICz..12...73S"
ABS    : "A discussion of hydrogen H&alpha;, H&beta;, H&gamma;, H&epsilon; and H&zeta; lines shows that in the flare investigated the Balmer lines were not broadened by the Stark effect, but most probably by a microturbulent motion, the characteristic velocity of which varied with the depth. The gradient of velocities was very expressive before and after the maximum phase and disappeared during the flash state. The calcium and helium lines must have been formed in other layers than the wings of the hydrogen lines, because the turbulent velocity for these lines was substantially smaller. The optical thickness of this flare was much less than that of the flare of July 30, 1958, and the number of two-quantum hydrogen atoms above 1 cm^2 of the base of the flare was 1.2&times;10^14 in the maximum phase. Balmer decrement leads to an electron temperature of the order of 10^5 degrees."

---
MARKER : "1960_list_of_flares"
TYPE   : "in_journal"
AUTHOR : "Kvicala, J., Hrebik, F., Letfus, V., Olmr, J., Svestka, Z., Krivsky, L."
TITLE  : "List of flares observed at Ondrejov observatory during the I.G.Y."
SERIAL : "Publikace Astronomicky Ustav, Ceskoslovenska Akademie Ved"
VOLUME : "43"
PAGE   : "(66 pages)"
PUBLISH: "Nakladatelstvi Ceskoslovenske Akademie Ved"
TOPKEY : "flares"
YEAR   : "1960-00"

---
MARKER : "1960_igy_145"
TYPE   : "in_proceedings"
AUTHOR : "Svestka, Z."
TITLE  : "Solar activity"
CTITLE : "Proc. International Geophysical Year and cooperation in Czechoslovakia, 1957-1959"
PAGE   : "145-168"
PUBLISH: "Nakladatelstvi, Ceskosloveneske Akademie Ved Praha"
YEAR   : "1960-00"
TOPKEY : "solar activity"
URL    : "http://adsabs.harvard.edu/abs/1960igyc.conf..145S"

---
MARKER : "1960_nature_187_224"
TYPE   : "in_journal"
AUTHOR : "Blaha, M., Kopecky, M., Svestka, Z."
TITLE  : "Measurement of magnetic fields in chromospheric flares"
SERIAL : "Nature"
VOLUME : "187 (4733)"
PAGE   : "224-225"
YEAR   : "1960-07"
DOI    : "10.1038/187224a0"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1960Natur.187..224B"
ABS    : "Spectra of two great chromospheric flares taken by the flare spectrograph at Ondrejov show an evident splitting of the D 1 emission line of Na I which is attributed to a magnetic field existing in that part of the chromosphere where the sodium lines are formed."

---
MARKER : "1960_baic_11_167"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Hydrogen spectum of the flare of July 30, 1959"
SERIAL : "Bull. Astron. Inst. Czech."
VOLUME : "11"
PAGE   : "167-170"
YEAR   : "1960-02"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1960BAICz..11..167S"
ABS    : "A discussion of hydrogen H&alpha;, H&beta;, H&gamma;, H&epsilon; and H&zeta; lines shows that the flare investigated lay in the lowest layers of the chromosphere, which is also indicated by an emission in the &lambda;3883 band of CN. Wings of the Balmer lines were formed in an optically very thick layer on the boundary between photosphere and chromosphere, where the number of free electrons exceeded 3&times;10^13 cm^-3. The excitation in this layer, however, was rahter low and the electron temperature did not exceed 7000&deg;. This basic layer, whose thickness can be estimated to less than 200 km, was overlain by a more extensive but less opaque region, where the excitation and electron temperature increased, while the electron density decreased with the increasing height. Cores of the Balmer lines, as well as metallic lines, the intensity of which in many cases substantially exceeded 100% of the continuum, were formed in this more extensive and more excited layer."

---
MARKER : "1959_baic_10_149"
TYPE   : "in_journal"
AUTHOR : "Valnicek, B., Letfus, V., Blaha, M., Svestka, Z., Seidl, Z."
TITLE  : "The flare spectrograph at Ondrejov"
SERIAL : "Bull. Astron. Inst. Czech"
VOLUME : "10"
PAGE   : "149-160"
YEAR   : "1959-09"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1959BAICz..10..149V"
ABS    : "This paper presents a description of the new solar spectrograph built at the Ondrejov Observatory in the year 1958. The spectrograph enables to take a series of simultaneous photographs of several spectral regions in short time intervals with a dispersion of at least 1 &Aring;/mm, so that it is highly suitable for the study of chromospheric flares and active prominences."

---
MARKER : "1959_baic_10_136"
TYPE   : "in_journal"
AUTHOR : "Letfus, V., Ruzickova, B., Svestka, Z."
TITLE  : "Catalogue of chromospheric flares observed at Ondrejov during the first half of the year 1957"
SERIAL : "Bull. Astron. Inst. Czech"
VOLUME : "10"
PAGE   : "136-144"
YEAR   : "1959-09"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1959BAICz..10..136L"
ABS    : "This paper is a continuation of three preceding catalogues, which contained flares observed at Ondrejov up to the end of the year 1956. Curves of the H&alpha; line-width changes for 268 flares observed during the first half of the year 1957 are plotted in Figures 1-3. The corresponding data about all these flares are summarized in the catalogue."

---
MARKER : "1959_baic_10_10"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Damping and Stark broadening of Balmer lines"
SERIAL : "Bull. Astron. Inst. Czech"
VOLUME : "10"
PAGE   : "10-12"
YEAR   : "1959-01"
URL    : "http://adsabs.harvard.edu/abs/1959BAICz..10...10S"
ABS    : "Using an approximate formula, we calculate the course of the absorption coefficient for the outer parts of the lines H&alpha;, H&beta;, H&gamma;, and H&delta;, if the number of free electrons is in the range of 10^10 to 10^14 cm^-3. The approximate formula used is compared with an exact calculation made for the H&alpha; line at temperature of 10,000&deg; and the number of free electrons equal to 10^13 cm^-3."

---
MARKER : "1958_nature_182_331"
TYPE   : "in_journal"
AUTHOR : "Blaha, M., Hruska, A., Svestka, Z., Vanysek, V."
TITLE  : "Polarization of light of the comets Arend-Roland (1956h) and Mrkos (1957d)"
SERIAL : "Nature"
VOLUME : "182 (4631)"
PAGE   : "331-332"
YEAR   : "1958-08"
DOI    : "10.1038/182331b0"
TOPKEY : "comet brightness"
URL    : "http://adsabs.harvard.edu/abs/1958Natur.182..331B"
ABS    : "Polarization of the total light of the Comets 1956h and 1957d was studied photographically by simultaneous exposures with three objectives and three 'Polaroids'. The planes of polarization of the three 'Polaroids' were at 120&deg;. 2-in. objectives were used at f/9 with Agfa 'Astro' panchromatic plates. The characteristic curve was determined by comparison with an exposed photometric wedge. Errors due to the instrument were measured by means of light from an artificial source, polarized to a known degree by reflexion from a glass surface. The error of the polarization determined is &plusmn;2.5 per cent."

---
MARKER : "1958_j_czech_astr_inst_35_97"
TYPE   : "in_journal"
AUTHOR : "Fritzova, L., Kopecky, M., Svestka, Z."
SERIAL : "J. Astronomical Institute of the Czechoslovak Academy of Sciences"
TITLE  : "Catalogue of great chromospheric flares and their terrestrial consequences"
VOLUME : "35"
PAGE   : "97-174"
PUBLISH: "Czechoslovak Academy of Sciences"
TOPKEY : "flares"
YEAR   : "1958-00"

---
MARKER : "1958_baic_9_178"
TYPE   : "in_journal"
AUTHOR : "Letfus, V., Ruzickova, B., Svestka, Z."
TITLE  : "Catalogue of chromospheric flares observed at Ondrejov during the years 1952-1956"
SERIAL : "Bull. Astron. Inst. Czech"
VOLUME : "9"
PAGE   : "178-190"
YEAR   : "1958-01"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1958BAICz...9..178L"
ABS    : "This paper is a continuation of the catalogue published by F. Link and D. Maskova, which contained flares observed at Ondrejov up to the year 1951. Curves of the H&alpha; line-width changes for 381 flares observed during 1952-1956 are plotted in Figures 1-5. The corresponding data about all these flares are summarized in the catalogue."

---
MARKER : "1958_baic_9_48"
TYPE   : "in_journal"
AUTHOR : "Budejicky, J., Svestka, Z."
TITLE  : "536 Mc/s radio events associated with chromospheric flares during the year 1956"
SERIAL : "Bull. Astron. Inst. Czech"
VOLUME : "9"
PAGE   : "48-60"
YEAR   : "1958-01"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1958BAICz...9...48B"
ABS    : "536 Mc/s events registered at Ondrejov during the year 1956 are compared with visual observations of chromospheric flares and with sudden ionospheric disturbances. 665 radio events of various types and 784 flares were observed during the investigated period. 129 events (19.4%) were found to be associated with flares or sudden ionospheric disturbances (S.I.D.'s) and 119 flares (15.2%) were accompanied with 536 Mc/s events. Percentage of coincidences increases with the increasing importance of flares. All events can be divided into two groups, I - typical flare events, and II - atypical flare events. From the events of the first group (major plus, major, minor plus, onset of noise storm, and group of bursts) more than 70% are associated with flares. This percentage is the lower limit of coincidences due to the interference of clouds at the visual observation. On the other hand, from the events of the second group (minor, base-level rise, series, and micro burst) only 12% are associated with flares. The percentage of accidental coincidences amounts to 6-12% for events of various types."

---
MARKER : "1957_unknown"
TYPE   : "report"
AUTHOR : "Svestka, Z."
TITLE  : "Physical conditions in chromospheric flares"
YEAR   : "1957-00"
TOPKEY : "flares"

---
MARKER : "1957_czech"
TYPE   : "book"
AUTHOR : "Svestka, Z."
TITLE  : "Fysikalni podminky V chromosferickych erupcich"
YEAR   : "1957-00"
PUBLISH: "Praha, Nakl. Ceskoslovenske akademie ved"
TOPKEY : "flares"

---
MARKER : "1957_baic_8_61"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z., Fritzova, L."
TITLE  : "Temperature conditions and the state of excitation in chromospheric flares"
SERIAL : "Bull. Astron. Inst. Czech"
VOLUME : "8"
PAGE   : "61-67"
YEAR   : "1957-01"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1957BAICz...8...61S"
ABS    : "We determine the number of hydrogen atoms in different quantum states in the flare from August 5, 1949, according to the measurements of the H&alpah;, H&gamma;, H&delta; H&epsilon;, and H&zeta; lines made by Mustel and Severny. The determination is based on measurements of the intensity in these lines and it differs from that obtained by the Russian authors, who discussed the intensity at the wings of the measured lines. We ascribe this difference to the fact that the back-radiation of the flare changes the physical conditions in photospheric layers beneath the flare, so that the absorption line created in these layers is deformed, and therefore the course of intensity at the wings of the emission lines must not be superponed on a normal absorption line profile. While Mustel and Severny have found an excitation close to the event of pure recombination, we find for the surface layers of the flare an excitation close to the equilibrium state for a temperature of about 6000&deg;. The source function must increase from the surface to the bottom of the flare as well as the kinetic temperature, which amounts to about 6000&deg; on the surface of the flare and increases to 9,000&deg;-10,000&deg; in its interior."

---
MARKER : "1956_czech"
TYPE   : "book"
AUTHOR : "Svestka, Z., Vanysek, V."
TITLE  : "Mezihvezdna hmota"
SERIAL : "Veda vsem. Sekce matem.-fys"
VOLUME : "14"
PAGE   : "(240 pages)"
YEAR   : "1956-00"
TOPKEY : "astrophysics"
PUBLISH: "Nakl. Ceskoslovenske akademie ved, Praha"

---
MARKER : "1956_baic_7_130"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "The optical thickness of flares and the broadening of Balmer lines in their spectra"
SERIAL : "Bull. Astron. Inst. Czechoslov."
VOLUME : "7"
PAGE   : "130-135"
YEAR   : "1956-02"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1956BAICz...7..130S"
ABS    : "It is proved that the optical thickness of chromospheric flares in the low lines of the Balmer series is very high. The H&alpha; line cannot be broadened by means of the Stark effect as the electron temperature needed would be extremely high. The right model of broadening the Balmer lines proves to be that one presented by Mustel and Severny, where the H&alpha; line is broadened by the radiation damping and the lines higher than H&beta; by the Stark effect."

---
MARKER : "1956_baic_7_30"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z., Fritzova, L."
TITLE  : "The width of H_alpha in solar flares"
SERIAL : "Bull. Astron. Inst. Czechoslov."
VOLUME : "7"
PAGE   : "30-32"
YEAR   : "1956-02"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1956BAICz...7...30S"
ABS    : "It is shown that the increase of H&alpha;-width in solar flares from the center to the limb of the solar disc found by Goldberg and collaborators, is a necessary consequence of the cosine-deformation of the visible area of flares. The increase in the number of flares with large line-width near the limb is due to an effect of selection."

---
MARKER : "1956_baic_7_9"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Several notes on the statistics of chromospheric flares"
SERIAL : "Bull. Astron. Inst. Czechoslov."
VOLUME : "7"
PAGE   : "9-18"
YEAR   : "1956-02"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1956BAICz...7....9S"
ABS    : "The paper contains a catalogue of monthly and yearly means of effective times of observation in spectrohelioscopes and spectroheliographs, together with the observed and real number of flares, observed and corrected &Sigma;q and the mean values of q per one flare. On the base of these statistical quantities a comparison of the flare-activity during the 17th and 18th solar cycles is carried out. It is shown that several phenomena, which are different in the two cycles, did not change in the minimum phase between the cycles but only in the year of maximum, 1947."

---
MARKER : "1954_czech"
TYPE   : "book"
AUTHOR : "Svestka, Z."
TITLE  : "Hvezdne atmosfery"
YEAR   : "1954-00"
TOPKEY : "stellar atmospheres"
PUBLISH: "Praha, Nakl. Ceskoslovenske akademie ved"
URL    : "http://adsabs.harvard.edu/abs/1954QB809.S85......"

---
MARKER : "1954_baic_5_91"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "The problem of a meteoritic dust layer in the Earth atmosphere"
SERIAL : "Bull. Astron. Inst. Czechoslov."
VOLUME : "5"
PAGE   : "91-98"
YEAR   : "1954-09"
TOPKEY : "Earth's shadow"
URL    : "http://adsabs.harvard.edu/abs/1954BAICz...5...91S"
ABS    : "The paper presents a critical study of Link's theory of fall and absorption influence of meteoritic particles in the atmosphere. Examining the influence of an atmospheric dust layer on the density of the earth shadow and the process of origin of meteoritic dust in the atmosphere we come to a conclusion that particles with radii &gt;1&mu; resulting from the Link theory cannot be a source of the absorption observed. Meteoritic dust probably is formed by smaller particles of the order 10^-5 - 10^-6 cm. It is shown that a study of sky-light polarisation might give a deciding answer to the investigated question. Study of the process of origin of meteoritic dust also shows that particles collected by Thomsen cannot be of interplanetary nature."

---
MARKER : "1954_baic_5_49"
TYPE   : "in_journal"
AUTHOR : "Fritzova, L., Pekny, Z., Svestka, Z."
TITLE  : "Secondary periods of long-periodic variables"
SERIAL : "Bull. Astron. Inst. Czechoslov."
VOLUME : "5"
PAGE   : "49-54"
YEAR   : "1954-06"
TOPKEY : "variable stars"
URL    : "http://adsabs.harvard.edu/abs/1954BAICz...5...49F"
ABS    : "It has been found that some long-period variables show secondary variations in extreme brightness and primary period. The stars R Auri, S Boot, R Caml, T Cass, U Pers, R Tria, S UMaj, T UMaj and R Virg are studied in detail."

---
MARKER : "1954_baic_5_4"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "A note on the dwarf flare stars"
SERIAL : "Bull. Astron. Inst. Czechoslov."
VOLUME : "5"
PAGE   : "4-6"
YEAR   : "1954-02"
TOPKEY : "flare stars"
URL    : "http://adsabs.harvard.edu/abs/1954BAICz...5....4S"
ABS    : "Flares observed on six dwarf Me-stars indicate that total-light variations become visible at the absolute visual magnitude +10^M and their amplitude increases with decreasing luminosity of these dwarfs. A list is appended, containing 50 dwarf Me-stars with M_v&gt;10 (6 known flare-stars included), which may be suspected from a variability of the flare-type."

---
MARKER : "1953_lunar_craters"
TYPE   : "report"
AUTHOR : "Bouska, J., Hrebik, F., Svestka, Z."
TITLE  : "Catalogue des crateres lunaire"
PAGE   : "107-115"
YEAR   : "1953-00"
TOPKEY : "lunar craters"
PUBLISH: "Publ. of the Astronomical Institute, Academy of Sciences of Czech Republic"

---
MARKER : "1953_czech"
TYPE   : "book"
AUTHOR : "Link, F., Svestka, Z."
TITLE  : "Slunce a jeho vlivy NA zemi"
YEAR   : "1953-00"
PAGE   : "(166 pages)"
PUBLISH: "Praha, Nakl. Ceskoslovenske akademie ved"
TOPKEY : "solar radiation"
URL    : "http://adsabs.harvard.edu/abs/1953QB521.L72......"

---
MARKER : "1953_baic_4_186"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Recurrent and revived active regions on the Sun"
SERIAL : "Bull. Astron. Inst. Czechoslov."
VOLUME : "4"
PAGE   : "186-192"
YEAR   : "1953-07"
TOPKEY : "active regions"
URL    : "http://adsabs.harvard.edu/abs/1953BAICz...4..186S"
ABS    : "Recurrent and revived active regions on the Sun are studied as to their flare-activity during the period 1935-1950. It is shown that the most important active centra are the revived and revived recurrent regions, which maintain high activity on the solar disc for several rotations. One of the most interesting peculiarities of the present cycle is a lack of these revived centra during its maximum phase. Because revived and recurrent centra contain about one half of all flares observed, this fact evidently is responsible for the low number of flares, n, in the present cycle (compared with the high values of R). Numerical formulae for the Waldmeier relation between n and R are given taking the recurrence into account."

---
MARKER : "1952_baic_3_1"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "The H_alpha emission from chromospheric flares VII: broadening of the line in the flash state"
SERIAL : "Bull. Astron. Inst. Czechoslov."
VOLUME : "3"
PAGE   : "1-6"
YEAR   : "1952-01"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1952BAICz...3....1S"
ABS    : "In this paper we continue the study of the dependence between central intensity and width of the H&alpha;-emission line emitted by flares. Attention is paid to the broadening of wings in the flash state and the way is shown in which this effect depends on the density of bright knots, temperature of the main radiating flare-area, and the ratio a_M/a_K. Resulting line-profiles show the characteristic narrow core and low broadened wings in good consent with observations."

---
MARKER : "1951_baic_2_165"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "The H_alpha-emission from chromospheric flares: central intensity and line-width"
SERIAL : "Bull. Astron. Inst. Czechoslov."
VOLUME : "2"
PAGE   : "165-172"
YEAR   : "1951-12"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1951BAICz...2..165S"
ABS    : "This paper brings a theoretical discussion of the relation between central intensity and line-width measured at the large chomospheric flare of August 5, 1949 (I 60). Assuming a hydrogenous source of radiation in thermodynamic equilibrium we take the Stark effect as the directing factor in forming the wings of the H&alpha;-emission line. The range of the discussed relation corresponding to the ceasing 'quiet' part of life of the flare, where our assumption is nearest to the truth, leads to a density of 10^14 to 2&times;10^14 hydrogen atoms per cm^3, inside the source of emission. This value shows that flares appear close to the basis of the chromosphere, where the temperature is comparable with the temperature of photosphere. To explain the enormous extension of wings in the 'flash' state we must conclude that the observed bright 'knots' responsible for this extension are denser and hotter than the main soure of flare-radiation. The density of these hot centra is found to be 10-100 times larger than inside the main source. The maximum temperature corresponding to the ideal state of thermodynamic equilibrium is found to be 11,200&deg; in the main source and 14,000&deg; in the hot centra of flare-emission. Deviations from the state of thermodynamic equilibrium, however, may enlarge these values of temperature in a measure, which cannot be estimated without further detailed discussion."

---
MARKER : "1951_baic_2_153"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "The H_alpha-emission from chromospheric flares: The flare of August 5, 1949"
SERIAL : "Bull. Astron. Inst. Czechoslov."
VOLUME : "2"
PAGE   : "153-155"
YEAR   : "1951-09"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1951BAICz...2..153S"
ABS    : "Observations made at Ondrejov complete the set of observations made at Greenwich, Arcetri, Muswell Hill, and Cambridge, and confirm the fact that the maximum of line-width appeared 3-4 minutes before the maximum of central intensity. The separation of the red- and blue-wing change leads to several interesting conclusions. The ascertained dependence of central intensity of line-width during the life of the flare may be used as the base of a further theoretical discussion."

---
MARKER : "1951_baic_2_150"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "The H_alpha-emission from chromospheric flares: expanding source of radiation"
SERIAL : "Bull. Astron. Inst. Czechoslov."
VOLUME : "2"
PAGE   : "150-153"
YEAR   : "1951-09"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1951BAICz...2..150S"
ABS    : "Waldmeier's explanations of the asymmetry of the H&alpha; emission line, i.e. a selfabsorption in an expanding source of radiative energy, is discussed and rejected. Several modifications of Waldmeier's original proposal are also examined and it is shown that no expansion process inside the source of flare-radiation can be responsible for the asymmetry observed and described in former parts of this series."

---
MARKER : "1951_baic_2_120"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "The H_alpha-emission from chromospheric flares: course of the asymmetry"
SERIAL : "Bull. Astron. Inst. Czechoslov."
VOLUME : "2"
PAGE   : "120-125"
YEAR   : "1951-05"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1951BAICz...2..120S"
ABS    : "The course of the asymmetry of the H&alpha;-emission line during the life of flares is studied in detail. It is shown that the presence of an asymmetrical Stark effect must probably be taken into consideration near the time of the flash-state, while the general course of the asymmetry does not withstand the assumption formerly accepted that absorption in rising chromospheric layers together with absorption in unhomogeneous clouds in the chromosphere is the main course of the investigated phenomenon. Absorption in surges is also briefly discussed."

---
MARKER : "1951_baic_2_100"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "The H_alpha-emission from chromospheric flares: general features of the asymmetry"
SERIAL : "Bull. Astron. Inst. Czechoslov."
VOLUME : "2"
PAGE   : "100-103"
YEAR   : "1951-02"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1951BAICz...2..100S"
ABS    : "This paper presents the first part of a study of the asymmetry of the H&alpha;-emission line in spectra of chromosheric flares. In contradiction of the results of Waldmeier and Ellison it is found that the asymmetry lasts for a longer time after the maximum intensity, and may be negative as well in late states of flares. The might and course of the asymmetry show that this phenomenon is probably caused by an absorption in moving clouds of H-atoms in the second state which are not identical with the Chapman's stream of corpuscules as has been supposed by Ellison and Kahn."

---
MARKER : "1951_baic_2_81"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "The H_alpha-emission from chromospheric flares: observations"
SERIAL : "Bull. Astron. Inst. Czechoslov."
VOLUME : "2"
PAGE   : "81-86"
YEAR   : "1951-02"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1951BAICz...2...81S"
ABS    : "The following series of papers studies several characteristic features of the H&alpha;-emission from chromospheric flares and uses them to draw some conclusions on the process of radiation of these solar phenomena. The present study is based on the rich material assembled at the station of the National Observatory at Ondrejov by different observers during the years 1947-1949, which is briefly summarized in this first part of the series presented. Several notes are also added concerning the method of measurement, its errors and effects, which occur at the observational work."

---
MARKER : "1950_baic_2_52"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "On a possible development of planetary nebulae"
SERIAL : "Bull. Astron. Inst. Czechoslov."
VOLUME : "2"
PAGE   : "52-56"
YEAR   : "1950-09"
URL    : "http://adsabs.harvard.edu/abs/1950BAICz...2...52S"
ABS    : "Using Zanstra's expansion hypothesis and the theoretical conclusions by Milne and Ambarzumian, a supposition is made that the distance of the ring of maximum brightness from the centre of the disk of a planetary nebula is a measure of age of these phenomenons, normal ring nebulae being at the end of the development curve. Good agreement with observation is found. Comparing the distances as given by Zanstra and Vorontsov-Velyaminov a change of M_n during the development is estimated. It is shown that an interstellar absorption 0.9-1.0 mg phot/1000 parsec must be taken into account to get the best agreement with data given by observation. Using the development curve finally obtained it is shown that the average velocity of expansion should increase roughly in the way theoretically predicted by Zanstra. A possible explanation of Wilson's problem of [Nev] lines in the nebular spectrum of NGC 2392 is indicated. Theoretical objections are briefly discussed in the last paragraph."

---
MARKER : "1950_baic_2_45"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "The reason of validity of the Bode's law"
SERIAL : "Bull. Astron. Inst. Czechoslov."
VOLUME : "2"
PAGE   : "45-46"
YEAR   : "1950-06"
TOPKEY : "Bode's law"
URL    : "http://adsabs.harvard.edu/abs/1950BAICz...2...45S"
ABS    : "Using Kuiper's law of planetary distances it is shown that the validity of Bode's law is accidental. A necessary condition for it is the distribution of mass in the planetary system"

---
MARKER : "1950_baic_2_41"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "A note on the brightness of lunar eclipses"
SERIAL : "Bull. Astron. Inst. Czechoslov."
VOLUME : "2"
PAGE   : "41-43"
YEAR   : "1950-06"
TOPKEY : "lunar eclipse"
URL    : "http://adsabs.harvard.edu/abs/1950BAICz...2...41S"
ABS    : "The dependence on solar activity, former found by Vaucouleurs, is corrected with regard to the influence of the moon's parallax. The possibility of a secondary dependence on the quantity of meteoric dust in the earth's atmosphere replaces the yearly periodicity former supposed."

---
MARKER : "1950_baic_2_6"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "On the variations of the enlargement of the Earth's shadow during the lunar eclipses"
SERIAL : "Bull. Astron. Inst. Czechoslov."
VOLUME : "2"
PAGE   : "6-7"
YEAR   : "1950-03"
TOPKEY : "Earth's shadow, lunar eclipse"
URL    : "http://adsabs.harvard.edu/abs/1950BAICz...2....6S"
ABS    : "There seems to exist a correlation between the relative enlargement of the earth's shadow and strong meteoric showers."

---
MARKER : "1949_baic_1_131"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "The influence of clouds on the density of the central part of the Earth's shadow"
SERIAL : "Bull. Astron. Inst. Czechoslov."
VOLUME : "1"
PAGE   : "131-135"
YEAR   : "1949-11"
URL    : "http://adsabs.harvard.edu/abs/1949BAICz...1..131S"
TOPKEY : "Earth's shadow"
ABS    : "This paper consists of two parts: (1) An investigation of the influence of clouds of different heights and transparencies on the density of the shadow. A method is described for easy computation of this effect in statistical works on lunar eclipses. (2) Further development of the writer's hypothesis on the origin of a relative clear up observed near the centre of the shadow is given. It is shown that clouds in maximum (equatorial) heights of about 7 km are of greatest importance for the investigated phenomenon."

---
MARKER : "1949_baic_1_123"
TYPE   : "in_journal"
AUTHOR : "Bouska, J., Svestka, Z."
TITLE  : "On the variation of the coma-diameter of Encke's Comet"
SERIAL : "Bull. Astron. Inst. Czechoslov."
VOLUME : "1"
PAGE   : "123-124"
YEAR   : "1949-10"
URL    : "http://adsabs.harvard.edu/abs/1949BAICz...1..123B"
TOPKEY : "comet nucleus"
ABS    : "In the present paper the coma-variations of the comet Encke are investigated. The amplitude of these variations during the years 1795-1947 was 3.5'. Variations of the coma-diameter are not in a correlation with the variations of the absolute brightness. On the contrary, there seems to exist a correlation between the coma-diameter and the solar activity. This phenomenon is, of course, very blank, and probably as great as the observation errors."

---
MARKER : "1949_baic_1_109"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "On the observed density of the Earth's shadow near its centre"
SERIAL : "Bull. Astron. Inst. Czechoslov."
VOLUME : "1"
PAGE   : "109-118"
YEAR   : "1949-10"
URL    : "http://adsabs.harvard.edu/abs/1949BAICz...1..109S"
TOPKEY : "Earth's shadow"
ABS    : "Observed densities of the earth's shadow during 11 photometrically investigated eclipses are compared with the theoretical values given in a former paper by the author. A striking relative clear up is found near the centre of the shadow, and this phenomenon is quantitatively investigated. It is shown that different heights of clouds in different latitudes are the most probable explanation of the effect observed."

---
MARKER : "1949_baic_1_100"
TYPE   : "in_journal"
AUTHOR : "Link, F., Svestka, Z."
TITLE  : "Eruption chromospherique du 23 decembre 1948"
SERIAL : "Bull. Astron. Inst. Czechoslov."
VOLUME : "1"
PAGE   : "100-102"
YEAR   : "1949-06"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1949BAICz...1..100L"
ABS    : "On donne un apercu des manifestations terrestres de la grande eruption chroospherique du 23 decembre 1948. Une eruption chromospherique d'importance 3+ a ete observee a Ondrejov peu apres midi (T.U.) a la date citee plus haut. On a pu suivre son evolution d'apres la largeur de la raie H&alpha; ainsi que ses manifestations terrestres d'apres nos enregistrements magnetiques et ionospheriques."

---
MARKER : "1949_baic_1_95"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "On the real number of solar flares"
SERIAL : "Bull. Astron. Inst. Czechoslov."
VOLUME : "1"
PAGE   : "95-98"
YEAR   : "1949-06"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1949BAICz...1...95S"
ABS    : "When we calculate the average number of solar flares really existing we must add the time of mean duration of flares to every separate time of observation. When we consider this fact, the former Waldmeier's number of flares will be reduced at a ratio of 0.7 : 1 and the percentage distribution of flares will also change. Further it is shown that the average hour number of observed flares depends substantially on the method of observation. Thus we can explain a discrepancy between the average numbers of flares found at different observatories during an hour of net time observation."

---
MARKER : "1949_baic_1_73"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "Observations of solar flares and high-speed prominences from July to December 1948"
SERIAL : "Bull. Astron. Inst. Czechoslov."
VOLUME : "1"
PAGE   : "73"
YEAR   : "1949-03"
TOPKEY : "flares"
URL    : "http://adsabs.harvard.edu/abs/1949BAICz...1...73S"
ABS    : "Maximum effective line-widths of the bright H&alpha; emission for 38 solar flares are given in Table I, and 9 measured curves of changes in line-widths are demonstrated in the figure enclosed."

---
MARKER : "1948_baic_1_29"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "The density of the Earth's shadow near its center"
SERIAL : "Bull. Astron. Inst. Czechoslov."
VOLUME : "1"
PAGE   : "29-32"
YEAR   : "1948-09"
TOPKEY : "Earth shadow"
URL    : "http://adsabs.harvard.edu/abs/1948BAICz...1...29S"
URL    : "http://articles.adsabs.harvard.edu/cgi-bin/nph-iarticle_query?bibcode=1948BAICz...1...29S&db_key=AST&page_ind=0&data_type=GIF&type=SCREEN_VIEW&classic=YES"
ABS    : "Paper has no abstract"

---
MARKER : "1948_baic_1_48"
TYPE   : "in_journal"
AUTHOR : "Svestka, Z."
TITLE  : "The illumination by diffusion in the center of the Earth's shadow"
SERIAL : "Bull. Astron. Inst. Czechoslov."
VOLUME : "1"
PAGE   : "48-51"
YEAR   : "1948-09"
TOPKEY : "Earth shadow"
URL    : "http://adsabs.harvard.edu/abs/1948BAICz...1...48S"
URL    : "http://articles.adsabs.harvard.edu/cgi-bin/nph-journal_query?volume=1&amp;plate_select=NO&amp;page=48&amp;plate=&amp;cover=&amp;journal=BAICz"
ABS    : "Paper has no abstract"