---
MARKER : "2014_apj_x_x"
TYPE   : "in_journal"
AUTHOR : "Yu, H.-S., Jackson, B.V., Buffington, A., Hick, P.P., Shimojo, M., Sako, N."
TITLE  : "The 3D analysis of Hinode polar jets using images from LASCO C2, the STEREO COR2 coronagraphs, and the Solar Mass Ejection Imager (SMEI)"
SERIAL : "Astrophys. J."
VOLUME : "XX"
PAGE   : "XX-XX"
YEAR   : "2014-02"
TOPKEY : "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"
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"
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 : "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"
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, 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"
AUTHOR : "Jackson, B.V., Buffington, A., Clover, J.M., Hick, P.P., Yu, H.-S., Bisi, M.M."
AFFIL  : "UCSD-CASS-SHPG; UCSD-CASS-SHPG; UCSD-CASS-SHPG; UCSD-CASS-SHPG; 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 : "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"
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, 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"
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"
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"
URL    : "http://www.worldscientific.com/doi/abs/10.1142/9789814405744_0007"
DOI    : "10.1142/9789814405744_0007"
TOPKEY : "IPS, 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"
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 : "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 : "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"
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 : "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 : "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_jastp_73_1317"
TYPE   : "in_journal"
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 : "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"
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 : "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 : "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"
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 : "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_apj_724_829"
TYPE   : "in_journal"
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 : "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"
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, 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 : "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"
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"
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, SMEI"

---
MARKER : "2010_solar_phys_265_233"
TYPE   : "in_journal"
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 : "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_265_257"
TYPE   : "in_journal"
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 : "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"
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"
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 : "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"
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 : "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"
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"
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"
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 : "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"
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 : "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 : "SMEI"

---
MARKER : "2010_sw12_aip_1216_355"
TYPE   : "in_proceedings"
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"
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"
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 : "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 : "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"
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 : "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 : "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"
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, 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 : "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 : "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 : "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 : "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 "
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 : "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"
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 : "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"
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 : "2008_jgr_113_a00a15"
TYPE   : "in_journal"
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 : "SMEI, CME"
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"
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 : "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 : "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 : "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 : "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 : "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_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 : "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_aspcs_385_167"
TYPE   : "in_proceedings"
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"
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 : "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"
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 : "SMEI, comet plasma tail, CME"
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_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 : "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 : "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_aat_26_477"
TYPE   : "in_proceedings"
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, 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_adv_geosci_st_14_161"
TYPE   : "in_proceedings"
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"
URL    : "http://ebooks.worldscinet.com/ISBN/9789812836205/9789812836205_0012.html"
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 : "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 : "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"
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 : "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"
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 : "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"
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"
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 : "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 : "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 : "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_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 : "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_jgr_112_a05106"
TYPE   : "in_journal "
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 : "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"
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 : "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"
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 : "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 : "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_jgr_111_a04s91"
TYPE   : "in_journal"
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 : "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 : "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_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 : "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"
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 : "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 : "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 : "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 : "2005_spie_59011b"
TYPE   : "in_proceedings"
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 : "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"
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 : "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"
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 : "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 : "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 "
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 : "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 Conference (Pune, India)"
VOLUME : "2"
PAGE   : "267-270"
YEAR   : "2005-08"
TOPKEY : "SMEI"
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 Conference (Pune, India)"
VOLUME : "1"
PAGE   : "165-168"
YEAR   : "2005-08"
TOPKEY : "SMEI"
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_spie_590118"
TYPE   : "in_proceedings"
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 : "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"
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 : "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_227_339"
TYPE   : "in_journal"
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"
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"
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 : "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 : "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 : "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"
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 : "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"
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"
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"
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_news"
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 : "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"
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 : "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_217_319"
TYPE   : "in_journal"
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 : "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"
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"
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"
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 : "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"
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"
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 : "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"
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_ursi_p1637"
TYPE   : "in_proceedings"
AUTHOR : "Hick, P., Jackson, B.V., Buffington, A."
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_eos_83_33"
TYPE   : "in_journal"
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 : "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"
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 : "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 : "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"
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_space_sci_rev_97_35"
TYPE   : "in_proceedings"
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"
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_asr_25_1875"
TYPE   : "in_proceedings"
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 spacecraft"
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_aip_sw9_471_565"
TYPE   : "in_proceedings"
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"
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, coronal"
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"
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"
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_solar_phys_182_179"
TYPE   : "in_journal"
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_spie_3442_77"
TYPE   : "in_proceedings"
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"
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_spie_3442_87"
TYPE   : "in_proceedings"
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"
DOI    : "10.1117/12.330246"
TOPKEY : "Helios spacecraft"
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_jgr_103_1991"
TYPE   : "in_journal"
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"
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_jgr_103_12049"
TYPE   : "in_journal"
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_soltip_3_207"
TYPE   : "in_proceedings"
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 : "1997_solar_phys_176_355"
TYPE   : "in_journal"
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_esa_sp_415_139"
TYPE   : "in_proceedings"
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"
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"
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 : "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"
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"
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"
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"
AUTHOR : "Webb, D.F., Jackson, B.V., Hick, P."
TYPE   : "in_proceedings"
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 spacecraft"

---
MARKER : "1996_iau_153_609"
TYPE   : "in_proceedings"
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"
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 : "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"
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 : "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"
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 spacecraft"
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"
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 : "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"
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"
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"
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 : "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"
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"
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"
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"
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 : "1995_colleferro"
AUTHOR : "Jackson, B.V., Buffington, A., Hick, P., Kahler, S.W., Keil, S.L., Altrock, R.C., Simnett, G.M., Webb, D.F."
TYPE   : "in_proceedings"
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 : "SMEI"

---
MARKER : "1995_solar_phys_161_331"
TYPE   : "in_journal"
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_esa_sp_373_199"
TYPE   : "in_proceedings"
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 spacecraft"
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"
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 : "1994_aasup_108_279"
TYPE   : "in_journal"
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_pltr_94_2040"
TYPE   : "report"
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 spacecraft"
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"
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 spacecraft, 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 : "1993_asr_13_71"
TYPE   : "in_proceedings"
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 spacecraft"
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"
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 spacecraft"
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_146_313"
TYPE   : "in_journal"
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 : "1992_sw7_187"
TYPE   : "in_proceedings"
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 spacecraft"
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"
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 : "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_aa_244_242"
TYPE   : "in_journal"
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 spacecraft"
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"
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 spacecraft"
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"
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 : "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 : "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_geophys_mono_54_291"
TYPE   : "in_proceedings"
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 : "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 : "1988_afgl_tr_88_0195"
TYPE   : "tech. report"
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 : "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."

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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 : "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."

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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."

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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."

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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"
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."

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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)."

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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"
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."

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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."

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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."