explanation      blue bibcodes open ADS page with paths to full text
Author name code: jackson
ADS astronomy entries on 2022-09-14
author:"Jackson, Bernard V." NOT =author:"Jackson, B."

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Title: ASHI, an All Sky Heliospheric Imager Designed to Maximize
    the Scientific Return from Structures Passing the Spacecraft
Authors: Jackson, Bernard; Buffington, Andrew; Kahler, Stephen; Bisi,
   Mario M.; Bracamontes, Matthew; Stephan, Ed; Volkow, Stuart; Quillian,
   Ron; Cota, Lucas; Leblanc, Philippe
2022cosp...44.1119J    Altcode:
  We have conceived, designed, and have evaluated components for an
  All-Sky Heliospheric Imager (ASHI), suitable for flight on future space
  missions. ASHI is currently manifested on a DoD Space Test Program ESPA
  ring in geosynchronous (GEO) orbit where high satellite communication
  downlink rates are relatively easy to provide. As a simple, light
  weight (<5kg), and relatively inexpensive instrument, the ASHI
  system has the principal objective of providing a minute-by-minute and
  day-by-day near real time acquisition of precision Thomson-scattering
  photometric maps of the inner heliosphere. The instrument's unique
  optical system is designed to view a hemisphere of sky starting a
  few degrees from the Sun. A key photometric specification for ASHI
  is 0.001 fractional differential photometry in one-degree sky bins
  at 90 degrees elongation that enables the three dimensional (3-D)
  reconstruction of heliospheric density extending outward from near
  the Sun. The ASHI system, unlike coronagraphs or planned heliospheric
  imagers, is intended to maximize the scientific return of heliospheric
  structures that pass the spacecraft. This will allow density structure
  measured in-situ to be extended outward into the surrounding plasma,
  and in GEO orbit this is Earth. This is especially important where
  recent high-resolution Solar Mass Ejection Imager (SMEI) and STEREO
  Heliospheric Imager (HI) analyses have shown CMEs have an evolving and
  "corrugated" structure when they pass nearby. An instrument similar to
  that of the full space-borne ASHI system will be tested late this summer
  on a NASA-sponsored topside balloon flight; a successful space-borne
  flight will have an order of magnitude more throughput than SMEI or
  the STEREO HI instrumentation, and thus provide a far better science
  and forecast capability than possible before.

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Title: STEREO A Heliospheric Imager and Interplanetary Scintillation
    Observations Now Provide Near Real Time 3-D High-Resolution Density
    and Velocity Reconstructions of the Inner Heliosphere
Authors: Jackson, Bernard; Buffington, Andrew; Bisi, Mario M.; Barnes,
   David; Tokumaru, Munetoshi; Bracamontes, Matthew; Davies, Jackie A.;
   Cota, Lucas
2022cosp...44.1085J    Altcode:
  We have recently adapted the UCSD Solar Mass Ejection Imager (SMEI)
  iterative tomography analyses for use with STEREO Heliospheric Imager
  (HI) data to provide 3-D reconstructed plasma densities of the
  inner heliosphere in the region viewed by these instruments. These
  analyses also include interplanetary scintillation (IPS) Earth-based
  instrumentation data from ISEE, Japan, to help provide more
  comprehensive analyses of both high-resolution density and velocity. As
  STEREO A approaches the Earth over the coming year, this provides an
  unprecedented ability to reconstruct densities in that portion of the
  inner heliosphere Earthward of the Sun, and allows an ahead-of-time
  prediction of plasma density properties in this region. Because we are
  using HI data with a long temporal base removed, both Stream Interaction
  Regions (SIRs) and Interplanetary Coronal Mass Ejections (ICMEs)
  are among the phenomena that can be revealed by the analyses. Here we
  present this near real time system operation that, albeit limited by
  the fact that the latency of the current STEREO HI scientific image
  data is three to five days, provides 3-D reconstructions of the plasma
  density and its determination. These densities can be obtained at any
  location throughout the inner heliospheric region imaged, and radially
  extrapolated outward from them. The reconstructions are updated every
  six hours, which is well within the time limit needed for actionable
  forecasts of the arrival of the fastest heliospheric structures at
  Earth. This system benchmarks computing needs for high-resolution 3-D
  reconstruction analyses of this type. It prototypes the forecasting
  capability for future similar spacecraft heliospheric imager instruments
  such as the NASA Small Explorer PUNCH, UCSD's All Sky Heliospheric
  Imager (ASHI), or the Lagrange (Vigil) Heliospheric Imager that are
  intended to be operated with a shorter data latency.

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Title: ASHI, an All Sky Heliospheric Imager Designed to Maximize
    the Scientific Return from Structures Passing the Spacecraft
Authors: Jackson, Bernard; Buffington, Andrew; Bracamontes, Matthew;
   Cota, Lucas; Volkow, Stuart; Hick, P.; Kahler, Stephen; Stephan, Ed;
   Leblanc, Philippe; Quillin, Ron; Bisi, Mario
2021AGUFMSH45E2407J    Altcode:
  We have conceived, designed, and evaluated components for an All-Sky
  Heliospheric Imager (ASHI), suitable for flight on future space
  missions. ASHI is currently manifested on a DoD Space Test Program
  ESPA ring in geosynchronous orbit where high satellite communication
  downlink rates are relatively easy to provide. As a simple, light
  weight (<5kg), and relatively inexpensive instrument, the ASHI
  system has the principal objective of providing a minute-by-minute and
  day-by-day near real time acquisition of precision photometric maps
  of the inner heliosphere. The instrument's optical system is designed
  to view a hemisphere of sky starting a few degrees from the Sun. A key
  photometric specification for ASHI is 0.1% differential photometry in
  one-degree sky bins at 90 degrees elongation that enables the three
  dimensional (3-D) reconstruction of heliospheric density extending
  outward from near the Sun. The ASHI system, unlike other operating or
  planned heliospheric imagers, is intended to maximize the scientific
  return of heliospheric structures that pass the spacecraft. This will
  allow density structure measured in-situ to be extended outward into
  the surrounding plasma. This is especially important at Earth where
  recent high-resolution Solar Mass Ejection Imager (SMEI) analyses have
  shown some CMEs with a corrugated structure when they pass Earth. We
  anticipate that velocity can also be determined from the 2-D sequence
  of images by following the motion of the background structures using
  correlation tracking techniques, and also using 3-D reconstruction
  techniques along with density. This should also help determine the
  extent to which this corrugated structure extends to CME velocity. An
  instrument similar to that of the full space-borne ASHI system has
  been tested this year on a NASA-sponsored topside balloon flight,
  and it is our intent that a successful space-borne flight make inroads
  into this result found in the SMEI analyses.

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Title: STEREO A HI Observations Now Provide Near Real Time
    High-Resolution 3-D Density Reconstructions of the Inner Heliosphere
Authors: Jackson, Bernard; Cota, Lucas; Baracamontes, Matthew;
   Buffington, Andrew; Davies, Jackie; Bisi, Mario
2021AGUFMSH15A2030J    Altcode:
  The STEREO spacecraft Heliospheric Imagers (HIs) were designed
  to view the region between Sun and Earth and thereby maximize the
  scientific return of heliospheric Thomson-scattering brightness data
  from a non-Earth perspective along the Sun-Earth line. We have recently
  adapted the UCSD Solar Mass Ejection Imager (SMEI) iterative tomography
  analyses for use with STEREO HI data to provide 3-D reconstructed
  plasma densities of the inner heliosphere in the region viewed by these
  instruments. Now, as STEREO A approaches the Earth, this provides an
  unprecedented ability to reconstruct densities in that portion of the
  inner heliosphere Earthward of the Sun, and allows an ahead-of-time
  prediction of plasma density properties at high resolution in this
  region. Because we are using HI data with a long temporal base removed,
  both Stream Interaction Regions (SIRs) and Interplanetary Coronal
  Mass Ejections (ICMEs) are among the phenomena that can be diagnosed
  in the analyses. Here we show this near real time system operation
  that, albeit limited by the fact the latency of the current STEREO HI
  scientific image data is three to five days, provides imagery of the
  plasma density and its measurement at various locations throughout the
  inner heliospheric region viewed. The reconstructions are updated every
  six hours, which is well within the time limit needed to forecast the
  arrival of the fastest heliospheric structures at Earth. This system
  benchmarks computing needs for high-resolution 3-D reconstruction
  analyses of this type, and prototypes the forecasting capability for
  future similar spacecraft heliospheric imager instruments operated
  with a shorter data latency.

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Title: BepiColombo Science Investigations During Cruise and Flybys
    at the Earth, Venus and Mercury
Authors: Mangano, Valeria; Dósa, Melinda; Fränz, Markus; Milillo,
   Anna; Oliveira, Joana S.; Lee, Yeon Joo; McKenna-Lawlor, Susan; Grassi,
   Davide; Heyner, Daniel; Kozyrev, Alexander S.; Peron, Roberto; Helbert,
   Jörn; Besse, Sebastien; de la Fuente, Sara; Montagnon, Elsa; Zender,
   Joe; Volwerk, Martin; Chaufray, Jean-Yves; Slavin, James A.; Krüger,
   Harald; Maturilli, Alessandro; Cornet, Thomas; Iwai, Kazumasa; Miyoshi,
   Yoshizumi; Lucente, Marco; Massetti, Stefano; Schmidt, Carl A.; Dong,
   Chuanfei; Quarati, Francesco; Hirai, Takayuki; Varsani, Ali; Belyaev,
   Denis; Zhong, Jun; Kilpua, Emilia K. J.; Jackson, Bernard V.; Odstrcil,
   Dusan; Plaschke, Ferdinand; Vainio, Rami; Jarvinen, Riku; Ivanovski,
   Stavro Lambrov; Madár, Ákos; Erdős, Géza; Plainaki, Christina;
   Alberti, Tommaso; Aizawa, Sae; Benkhoff, Johannes; Murakami, Go;
   Quemerais, Eric; Hiesinger, Harald; Mitrofanov, Igor G.; Iess, Luciano;
   Santoli, Francesco; Orsini, Stefano; Lichtenegger, Herbert; Laky,
   Gunther; Barabash, Stas; Moissl, Richard; Huovelin, Juhani; Kasaba,
   Yasumasa; Saito, Yoshifumi; Kobayashi, Masanori; Baumjohann, Wolfgang
2021SSRv..217...23M    Altcode:
  The dual spacecraft mission BepiColombo is the first joint mission
  between the European Space Agency (ESA) and the Japanese Aerospace
  Exploration Agency (JAXA) to explore the planet Mercury. BepiColombo
  was launched from Kourou (French Guiana) on October 20th, 2018, in
  its packed configuration including two spacecraft, a transfer module,
  and a sunshield. BepiColombo cruise trajectory is a long journey
  into the inner heliosphere, and it includes one flyby of the Earth
  (in April 2020), two of Venus (in October 2020 and August 2021), and
  six of Mercury (starting from 2021), before orbit insertion in December
  2025. A big part of the mission instruments will be fully operational
  during the mission cruise phase, allowing unprecedented investigation
  of the different environments that will encounter during the 7-years
  long cruise. The present paper reviews all the planetary flybys and
  some interesting cruise configurations. Additional scientific research
  that will emerge in the coming years is also discussed, including the
  instruments that can contribute.

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Title: Impact of Inner Heliospheric Boundary Conditions on Solar
    Wind Predictions at Earth
Authors: Gonzi, Siegfried; Weinzierl, M.; Bocquet, F. -X.; Bisi,
   M. M.; Odstrcil, D.; Jackson, B. V.; Yeates, A. R.; Jackson, D. R.;
   Henney, C. J.; Nick Arge, C.
2021SpWea..1902499G    Altcode:
  Predictions of the physical parameters of the solar wind at Earth are
  at the core of operational space weather forecasts. Such predictions
  typically use line-of-sight observations of the photospheric magnetic
  field to drive a heliospheric model. The models Wang-Sheeley-Arge
  (WSA) and ENLIL for the transport in the heliosphere are commonly used
  for these respective tasks. Here we analyze the impact of replacing
  the potential field coronal boundary conditions from WSA with two
  alternative approaches. The first approach uses a more realistic
  nonpotential rather than potential approach, based on the Durham Magneto
  Frictional Code (DUMFRIC) model. In the second approach the ENLIL
  inner boundary conditions are based on Inter Planetary Scintillation
  observations (IPS). We compare predicted solar wind speed, plasma
  density, and magnetic field magnitude with observations from the WIND
  spacecraft for two 6-month intervals in 2014 and 2016. Results show
  that all models tested produce fairly similar output when compared
  to the observed time series. This is not only reflected in fairly low
  correlation coefficients (<0.3) but also large biases. For example,
  for solar wind speed some models have average biases of more than 150
  km/s. On a positive note, the choice of coronal magnetic field model has
  a clear influence on the model results when compared to the other models
  in this study. Simulations driven by IPS data have a high success rate
  with regard to detection of the high speed solar wind. Our results also
  indicate that model forecasts do not degrade for longer forecast times.

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Title: Nonthermal electrons revealed by LOFAR
Authors: Zucca, Pietro; Pellizzoni, Alberto; Krankowski, Andrzej;
   Rothkaehl, Hanna; Mann, Gottfried; Vocks, Christian; Magdalenic,
   Jasmina; Marque, Christophe; Jackson, Bernard; Fallows, Richard;
   Tomasik, Lukasz; Hamish; Reid, A. S.; Gallagher, Peter; Vourlidas,
   Angelos; Bisi, Mario M.; Carley, Eoin; Matyjasiak, Barbara; Kozarev,
   Kamen; Dabrowski, Bartosz; Morosan, Diana; Tiburzi, Caterina; Chang,
   Peijin
2021cosp...43E1065Z    Altcode:
  During solar flares and CMEs, the corona is heated, plasma motion,
  waves and shocks are ignited, and particles are accelerated. The
  accelerated particles propagate through the solar corona causing a
  variety of plasma instabilities that lead to enhanced non-thermal
  radio emission, known as "radio bursts". By studying radio-bursts'
  characteristics we can gain insight into the properties of energetic
  particles and the ambient coronal plasma, and the properties of particle
  acceleration mechanisms, such as magnetic reconnection and/or shocks
  in the solar atmosphere. The Low Frequency aRray (LOFAR) can be used
  to study the fundamental plasma physics of solar radio bursts with
  unprecedented time resolution in dynamic spectra, as well as with
  both interferometric imaging and tied array imaging. In this talk, an
  overview of recent results obtained with the LOFAR telescope will be
  given, including observations of a different variety of radio bursts
  such as type II, III and IV. These observations were performed with
  simultaneous beam formed and interferometric imaging, resulting in
  unprecedented special resolution with baselines up to ~120 km. Finally,
  we will present the plan for future observations and the remaining
  challenges of solar-heliospheric low-frequency observations.

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Title: Iterative Interplanetary Scintillation (IPS) Analyses During
    the Parker Solar Probe Close Solar Solar Passes
Authors: Jackson, Bernard; Hick, P.; Buffington, Andrew; Fallows,
   Richard; Odstrcil, Dusan; Bisi, Mario M.; Cota, Lucas; Tokumaru,
   Munetoshi
2021cosp...43E.947J    Altcode:
  We at the University of California, San Diego (UCSD) have developed a
  time-dependent three-dimensional (3-D) reconstruction technique that
  provides volumetric maps of density and velocity by iteratively fitting
  a kinematic or the ENLIL 3-D MHD model to interplanetary scintillation
  (IPS) observations. This system is compared with NOAA- and NASA-provided
  in-situ spacecraft measurements, and is used for real time predictions
  of solar wind parameters at Earth or globally (see the UCSD website
  https://ips.ucsd.edu). Currently used with data from ISEE, Japan, we
  have also integrated this system with data from Worldwide IPS Stations
  (WIPSS) network groups to increase both spatial and temporal coverage
  when these data are available. Some of these stations, especially
  LOFAR, centered in the Netherlands, currently operate in "campaign"
  mode only during periods of interest when the Parker Solar Probe (PSP)
  makes close passes to the Sun. The UCSD 3-D iterative reconstruction
  technique is unique in its ability to provide a low-resolution seamless
  extension of density and velocity parameters measured in situ, outward
  into the surrounding interplanetary medium at the resolution of the
  volumetric data. We here present analyses using archival data sets
  from both ISEE and LOFAR, that also include both kinematic and ENLIL
  models during PSP close passes of the Sun. These analyses also show
  the location of Solar Orbiter within the 3-D reconstructed volumes.

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Title: ASHI: An All Sky Heliospheric Imager using Thomson-scattered
    Sunlight to Enable Near-Earth 3-D Plasma Reconstruction and Forecasts
Authors: Jackson, Bernard; Hick, P.; Buffington, Andrew; Kahler,
   Stephen; Bisi, Mario M.; Bracamontes, Matthew; Volkow, Stuart; Adriany,
   Kyle; Leblanc, Philippe; Stephan, Ed
2021cosp...43E.745J    Altcode:
  We have conceived, designed, and are now evaluating components for an
  All-Sky Heliospheric Imager (ASHI), suitable to fly on future NASA
  or DoD missions. ASHI's principal objective is the minute-by-minute
  and day-by-day acquisition of a precision photometric map of the
  inner heliosphere. The instrument's optical system is designed views a
  hemisphere of sky starting a few degrees from the Sun. Two such imagers
  on a single spacecraft, or a single imager whose spacecraft has a
  180$^\circ$ rotation, can view nearly the whole sky. A key photometric
  specification for ASHI is 0.1% differential photometry in a one-degree
  sky bin at 90$^\circ$ elongation. This enables the three dimensional
  (3-D) reconstruction of heliospheric density starting from near the Sun
  and extending outward, with updates as heliospheric structures approach,
  and pass the spacecraft. Velocity can also be ascertained from the 2-D
  sequence of images, by following the motion of the background structures
  using correlation tracking techniques. Solar Mass Ejection Imager (SMEI)
  analyses using data from 2003 to 2011 have demonstrated the success
  of this technique to provide density reconstructions: applying this to
  ASHI data will yield an order-of-magnitude improvement in 3-D density
  reconstructions (better than 2 x 2 degrees in latitude and longitude,
  and a 2-hour time resolution near the spacecraft). Here we present the
  latest results of the ASHI laboratory evaluations, nighttime full-sky
  tests of the instrument data sets, and the instrument construction
  to date.

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Title: A Ground-Based Heliospheric Observatory for Space Weather: The
    Worldwide Interplanetary Scintillation (IPS) Stations (WIPSS) Network
Authors: Bisi, Mario M.; Pacini, Alessandra; Aguilar-Rodriguez,
   Ernesto; Tokumaru, Munetoshi; Gonzalez-Esparza, Americo; Jackson,
   Bernard; Fallows, Richard; Fujiki, Kenichi; Yan, Yihua; Manoharan,
   Periasamy K.; Chashei, Igor; Tyulbashev, Sergei; Iwai, Kazumasa;
   Barnes, David; Chang, Oyuki; Robertson, Stuart
2021cosp...43E2370B    Altcode:
  The technique of using interplanetary scintillation (IPS) is unique
  technique in that allows for the determination of outflow velocity as
  well as a proxy for plasma density to be undertaken throughout both
  the corona and inner heliosphere depending on observing frequency. The
  results are often used as input to space-weather forecast/prediction
  programmes and models when data are sufficient (both in the temporal
  and spatial domains) as well as having a large scientific research
  value (true of long-duration observations, individual observations,
  and many days/weeks of observations). There is now a defined IPS Common
  Data Format (IPSCDFv1.1) which is being implemented by the majority
  of the IPS community. By combining the results from multiple observing
  locations around the globe where observations are undertaken throughout
  the day at each place, we can increase both the temporal and spatial
  coverage across the whole of the inner heliosphere. We are also able
  to probe different coronal/heliospheric regions from near to the Sun
  all the way out to beyond the orbit of the Earth. Observations of IPS
  also provide excellent opportunities to enhance collaborations between
  developed and developing countries thanks to the locations of many of
  the IPS-capable systems currently in use or under development. The
  Worldwide IPS Stations (WIPSS) Network brings together both the
  global real-/near-real-time (for space weather forecasting) and
  the scientific-/campaign-based systems (for space weather science)
  capable IPS observatories with well-developed and tested analyses
  techniques being unified across all single-site systems (such as MEXART,
  Pushchino, and Ooty) and cross-calibrated to the multi-site ISEE system
  (as well as learning from the scientific-based systems such as EISCAT,
  LOFAR, and the MWA). This is enhanced by using using IPSCDFv1.0 or
  IPSCDFv1.1. A WIPSS website has been developed by the MEXART group
  and was showcased in late 2018 where updates are currently being
  implemented. Here we will present an overview of the WIPSS Network
  along with some scientific highlights (where appropriate), and we will
  include any progress to date on initialising the real-time capabilities
  of WIPSS as well as any foreseen challenges (political, scientific,
  and financial) going forward.

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Title: Results from the LOFAR coordination with PSP
Authors: Zucca, Pietro; Pellizzoni, Alberto; Krankowski, Andrzej;
   Rothkaehl, Hanna; Mann, Gottfried; Vocks, Christian; Magdalenic,
   Jasmina; Marque, Christophe; Jackson, Bernard; Fallows, Richard;
   Tomasik, Lukasz; Miteva, Rositsa; Hamish; Reid, A. S.; Gallagher,
   Peter; Vourlidas, Angelos; Bisi, Mario M.; Carley, Eoin; Matyjasiak,
   Barbara; Kozarev, Kamen; Dabrowski, Bartosz; Morosan, Diana; Tiburzi,
   Caterina; Zhabngm, Peijin
2021cosp...43E.945Z    Altcode:
  Understanding and modelling the complex state of the Sun-solar
  wind-magnetosphere-ionosphere-thermosphere system, requires a
  comprehensive set of multiwavelength observations. LOFAR has unique
  capabilities in the radio domain. Some examples of these include: a)
  the ability to take high-resolution solar dynamic spectra and radio
  images of the Sun; b) observing the scintillation (interplanetary
  scintillation - IPS) of distant, compact, astronomical radio sources
  to determine the density, velocity and turbulence structure of the
  solar wind; and c) the use of Faraday rotation as a tool to probe
  the interplanetary magnetic-field strength and direction. However, to
  better understand and predict how the Sun, its atmosphere, and more
  in general the Heliosphere works and impacts Earth, the combination
  of in-situ spacecraft measurements and ground-based remote-sensing
  observations of coronal and heliospheric plasma parameters is extremely
  useful. Ground-based observations can be used to infer a global
  picture of the inner heliosphere, providing the essential context into
  which in-situ measurements from spacecraft can be placed. Conversely,
  remote-sensing observations usually contain information from extended
  lines of sight, with some deconvolution and modelling necessary to build
  up a three-dimensional (3-D) picture. Precise spacecraft measurements,
  when calibrated, can provide ground truth to constrain these models. The
  PSP mission is observing the solar corona and near-Sun interplanetary
  space. It has a highly-elliptical orbit taking the spacecraft as close
  as nearly 36 solar radii from the Sun centre on its first perihelion
  passage, and subsequent passages ultimately reaching as close as 9.8
  solar radii. Four instruments are on the spacecraft's payload: FIELDS
  measuring the radio emission, electric and magnetic fields, Poynting
  flux, and plasma waves as well as the electron density and temperature;
  ISOIS measuring energetic electrons, protons, and heavy ions in the
  energy range 10 keV-100 MeV; SWEAP measuring the density, temperature,
  and flow speed of electrons, protons, and alphas in the solar wind;
  and finally, WISPR imaging coronal streamers, coronal mass ejections
  (CMEs), their associated shocks, and other solar wind structures in the
  corona and near-Sun interplanetary space, and provide context for the
  other three in-situ instruments. In this talk, several results of the
  joint LOFAR/PSP campaign will be presented, including fine structures
  of radio bursts, localization and kinematics of propagating radio
  sources in the heliosphere, and the challenges and plans for future
  observing campaigns including PSP and Solar Orbiter.

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Title: UCSD Iterative Tomography Analyses Applied to STEREO HI
    Observations
Authors: Jackson, B. V.; Davies, J. A.; Bisi, M. M.; Cota, L. V.;
   Buffington, A.; Hick, P. P.
2020AGUFMSH0280007J    Altcode:
  The STEREO spacecraft provide heliospheric imaging systems
  particularly designed to maximize the scientific return of heliospheric
  Thomson-scattering brightness data from a non-Earth perspective. To
  aid in this analysis we have adapted the UCSD iterative tomography
  analyses for use with STEREO Heliospheric Imager observations to
  provide plasma densities of the inner heliosphere. These analyses
  show all manner of solar wind features with unprecedented precision-
  resolutions of a few degrees in latitude and longitude, solar distances
  of a few hundredths of an AU, and temporal cadences of about one hour
  in regions viewed by these instruments. Included in these are Stream
  Interaction Regions (SIRs) and Interplanetary Coronal Mass Ejections
  (ICMEs). These structures include shocked plasma density enhancements
  in front of SIRs and ICMEs, enhanced density in SIRs and in slow ICME
  sheath regions. They also show plasma voids in regions behind SIRs and
  ICMEs. In this analysis we look carefully at the shape and evolution of
  several plasma voids behind ICMEs as they evolve outward from close to
  the solar surface until they reach 1 AU where they are measured in situ.

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Title: Iterative Tomography: A Key to Providing Time- dependent
    3-D Reconstructions of the Inner Heliosphere and the Unification of
    Space Weather Forecasting Techniques
Authors: Jackson, Bernard V.; Buffington, Andrew; Cota, Lucas;
   Odstrcil, Dusan; Bisi, Mario M.; Fallows, Richard; Tokumaru, Munetoshi
2020FrASS...7...76J    Altcode:
  Over several decades UCSD has developed and continually updated a
  time dependent iterative three-dimensional (3-D) reconstruction
  technique to provide global heliospheric parameters - density,
  velocity, and component magnetic fields. For expediency, this has used
  a kinematic model as a kernel to provide a fit to either interplanetary
  scintillation (IPS) or Thomson-scattering observations. This technique
  has been used in near real time over this period, employing Institute
  for Space-Earth Environmental Research (ISEE), Japan IPS data to predict
  the propagation of these parameters throughout the inner heliosphere. We
  have extended the 3-D reconstruction analysis to include other IPS
  Stations around the Globe in a Worldwide Interplanetary Scintillation
  Stations (WIPSS) Network. In addition, we also plan to resurrect the
  Solar Mass Ejection Imager (SMEI) Thomson-scattering analysis as a
  basis for 3-D analysis to be used by the latest NASA Small Explorer
  heliospheric imagers of the Polarimeter to Unify the Corona and
  Heliosphere (PUNCH) mission, the All Sky Heliospheric Imager (ASHI),
  and other modern wide-field imagers. Better data require improved
  Heliospheric modeling that incorporates non-radial transport of
  heliospheric flows, and shock processes. Looking ahead to this,
  we have constructed an interface between the 3-D reconstruction
  tomography and 3-D MHD models, and currently include the ENLIL model
  as a kernel in the reconstructions to provide this fit. In short,
  we are now poised to provide all of these innovations in a next step:
  to include them for planned ground-based and spacecraft instruments,
  all to be combined into a truly global 3-D heliospheric system which
  utilizes these aspects in their data and modeling.

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Title: VizieR Online Data Catalog: Interplanetary scintillation at
    79 and 158MHz (Morgan+, 2018)
Authors: Morgan, J. S.; Macquart, J. -P.; Ekers, R.; Chhetri, R.;
   Tokumaru, M.; Manoharan, P. K.; Tremblay, S.; Bisi, M. M.; Jackson,
   B. V.
2020yCat..74732965M    Altcode:
  In order to allow multifrequency Interplanetary Scintillation (IPS)
  analysis, it was decided to split the MWA's 30.72MHz of instantaneous
  bandwidth into two bands, spaced approximately a factor of two apart in
  frequency. Within the MWA observing band, there is 15MHz of bandwidth
  directly below the FM broadcast band centred on 79MHz. An observing
  frequency of 158MHz, double the lower band frequency, is close to the
  centre of the MWA's usable band and gives a good trade-off between
  sensitivity, angular resolution, and field of view. <P />(2 data files).

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Title: Investigating Mercury's Environment with the Two-Spacecraft
    BepiColombo Mission
Authors: Milillo, A.; Fujimoto, M.; Murakami, G.; Benkhoff, J.; Zender,
   J.; Aizawa, S.; Dósa, M.; Griton, L.; Heyner, D.; Ho, G.; Imber,
   S. M.; Jia, X.; Karlsson, T.; Killen, R. M.; Laurenza, M.; Lindsay,
   S. T.; McKenna-Lawlor, S.; Mura, A.; Raines, J. M.; Rothery, D. A.;
   André, N.; Baumjohann, W.; Berezhnoy, A.; Bourdin, P. A.; Bunce,
   E. J.; Califano, F.; Deca, J.; de la Fuente, S.; Dong, C.; Grava,
   C.; Fatemi, S.; Henri, P.; Ivanovski, S. L.; Jackson, B. V.; James,
   M.; Kallio, E.; Kasaba, Y.; Kilpua, E.; Kobayashi, M.; Langlais, B.;
   Leblanc, F.; Lhotka, C.; Mangano, V.; Martindale, A.; Massetti, S.;
   Masters, A.; Morooka, M.; Narita, Y.; Oliveira, J. S.; Odstrcil, D.;
   Orsini, S.; Pelizzo, M. G.; Plainaki, C.; Plaschke, F.; Sahraoui, F.;
   Seki, K.; Slavin, J. A.; Vainio, R.; Wurz, P.; Barabash, S.; Carr,
   C. M.; Delcourt, D.; Glassmeier, K. -H.; Grande, M.; Hirahara, M.;
   Huovelin, J.; Korablev, O.; Kojima, H.; Lichtenegger, H.; Livi, S.;
   Matsuoka, A.; Moissl, R.; Moncuquet, M.; Muinonen, K.; Quèmerais,
   E.; Saito, Y.; Yagitani, S.; Yoshikawa, I.; Wahlund, J. -E.
2020SSRv..216...93M    Altcode: 2022arXiv220213243M
  The ESA-JAXA BepiColombo mission will provide simultaneous measurements
  from two spacecraft, offering an unprecedented opportunity to
  investigate magnetospheric and exospheric dynamics at Mercury as
  well as their interactions with the solar wind, radiation, and
  interplanetary dust. Many scientific instruments onboard the two
  spacecraft will be completely, or partially devoted to study the
  near-space environment of Mercury as well as the complex processes
  that govern it. Many issues remain unsolved even after the MESSENGER
  mission that ended in 2015. The specific orbits of the two spacecraft,
  MPO and Mio, and the comprehensive scientific payload allow a wider
  range of scientific questions to be addressed than those that could
  be achieved by the individual instruments acting alone, or by previous
  missions. These joint observations are of key importance because many
  phenomena in Mercury's environment are highly temporally and spatially
  variable. Examples of possible coordinated observations are described in
  this article, analysing the required geometrical conditions, pointing,
  resolutions and operation timing of different BepiColombo instruments
  sensors.

---------------------------------------------------------
Title: The UCSD Iterative Interplanetary Scintillation (IPS) Analysis
    Using an ENLIL 3-D MHD Model Kernel
Authors: Jackson, B. V.; Odstrcil, D.; Hick, P. P.; Buffington, A.;
   Tokumaru, M.; Bisi, M. M.
2019AGUFMSH43D3362J    Altcode:
  We at the University of California, San Diego (UCSD) have developed a
  time-dependent three-dimensional (3-D) reconstruction technique that
  provides volumetric maps of density and velocity by iteratively
  fitting 3-D MHD models to interplanetary scintillation (IPS)
  observations. This system is compared with NOAA- and NASA-provided
  in-situ spacecraft measurements, and is now being evaluated for use in
  real time predictions of solar wind parameters (see the UCSD website
  https://ips.ucsd.edu/ENLIL_prediction), in order to validate it in
  various operating conditions. Unlike previous UCSD kinematic modeling,
  this new tomographic analysis with a 3-D MHD kernel now includes
  shock processes and the non-radial transport of structures from an
  inner-boundary source surface placed at 0.1 AU. Magnetic fields are
  extrapolated outward from the solar surface to support the iterative
  procedure, and are shown to provide a low resolution several-day advance
  prediction of GSM Bz and geomagnetic storms. Used currently with data
  from ISEE, Japan, we have also integrated this system for use with data
  from Worldwide IPS Stations (WIPSS) network groups to increase both
  spatial and temporal coverage when these data are available. Some
  of these stations, especially LOFAR centered in the Netherlands,
  currently operate in "campaign" mode only during periods of interest
  when current and upcoming NASA and ESA spacecraft (Parker Solar Probe,
  BepiColombo, Solar Orbiter) make close passes to the Sun or planetary
  encounters. Here, the UCSD 3-D iterative reconstruction technique is
  unique in its ability to provide a low-resolution seamless extension
  of density and velocity parameters measured in situ outward into the
  surrounding interplanetary medium.

---------------------------------------------------------
Title: ASHI: An All Sky Heliospheric Imager to Provide Space Weather
    Forecasting Using Thomson-Scattered Sunlight
Authors: Jackson, B. V.; Buffington, A.; Leblanc, P.; Bracamontes,
   M.; Foroughi-Shafiei, S.; Edara, J.; Hick, P. P.; Bisi, M. M.
2019AGUFMSH33C3369J    Altcode:
  We have conceived, designed, and are now evaluating components
  for an All-Sky Heliospheric Imager (ASHI), to fly on future NASA
  missions. ASHI's principal objective is the minute-by-minute and
  day-by-day acquisition of a precision photometric map of the inner
  heliosphere. The instrument's optical design views a hemisphere of
  sky starting a few degrees from the Sun. Two such instruments on a
  single spacecraft, or a single instrument if the spacecraft has a
  180 degree rotation, can view nearly the whole sky. A key photometric
  specification for ASHI is 0.1% differential photometry in a one-degree
  sky bin at 90 degrees elongation. This enables the three dimensional
  (3-D) reconstruction of heliospheric density starting from near the
  Sun and extending outward, with updates as heliospheric structures
  approach, and pass the spacecraft. Velocity can also be ascertained
  from the imagery in 3-D, by following the motion of the background
  structures using correlation tracking techniques. SMEI analyses have
  demonstrated the success of this technique: a similar analysis for
  ASHI data will yield an order-of-magnitude improvement in 3-D density
  reconstructions (better than 2 x 2 degrees in latitude, and longitude,
  and a 2-hour time resolution near the spacecraft). Here we will present
  the latest results of the ASHI laboratory evaluations, and nighttime
  full-sky tests of the instrument data sets.

---------------------------------------------------------
Title: Validation of the Alfvén Wave Solar Atmosphere Model (AWSoM)
    with Observations from the Low Corona to 1 au
Authors: Sachdeva, Nishtha; van der Holst, Bart; Manchester, Ward B.;
   Tóth, Gabor; Chen, Yuxi; Lloveras, Diego G.; Vásquez, Alberto M.;
   Lamy, Philippe; Wojak, Julien; Jackson, Bernard V.; Yu, Hsiu-Shan;
   Henney, Carl J.
2019ApJ...887...83S    Altcode: 2019arXiv191008110S
  We perform a validation study of the latest version of the Alfvén
  Wave Solar atmosphere Model (AWSoM) within the Space Weather Modeling
  Framework. To do so, we compare the simulation results of the model
  with a comprehensive suite of observations for Carrington rotations
  representative of the solar minimum conditions extending from the
  solar corona to the heliosphere up to the Earth. In the low corona
  (r &lt; 1.25 {\text{}}{R}<SUB>⊙ </SUB>), we compare with EUV
  images from both Solar-Terrestrial Relations Observatory-A/EUVI
  and Solar Dynamics Observatory/Atmospheric Imaging Assembly and to
  three-dimensional (3D) tomographic reconstructions of the electron
  temperature and density based on these same data. We also compare the
  model to tomographic reconstructions of the electron density from
  Solar and Heliospheric Observatory/Large Angle and Spectrometric
  Coronagraph observations (2.55 &lt; r &lt; 6.0{\text{}}{R}<SUB>⊙
  </SUB>). In the heliosphere, we compare model predictions of solar wind
  speed with velocity reconstructions from InterPlanetary Scintillation
  observations. For comparison with observations near the Earth, we use
  OMNI data. Our results show that the improved AWSoM model performs
  well in quantitative agreement with the observations between the inner
  corona and 1 au. The model now reproduces the fast solar wind speed
  in the polar regions. Near the Earth, our model shows good agreement
  with observations of solar wind velocity, proton temperature, and
  density. AWSoM offers an extensive application to study the solar
  corona and larger heliosphere in concert with current and future solar
  missions as well as being well suited for space weather predictions.

---------------------------------------------------------
Title: The Worldwide Interplanetary Scintillation (IPS) Stations
(WIPSS) Network: A Ground-Based Heliospheric Observatory for Science
    and Space Weather
Authors: Bisi, M. M.; Jackson, B. V.; Gonzalez-Esparza, A.;
   Aguilar-Rodriguez, E.; Tokumaru, M.; Fallows, R. A.; Chang, O.; Abe
   Pacini, A.; Chashei, I. V.; Tyul'bashev, S. A.; Yan, Y.; Iwai, K.;
   Jangsuk, C.; Fujiki, K.; Manoharan, P. K.; Barnes, D.
2019AGUFMSA11C3233B    Altcode:
  Interplanetary Scintillation (IPS) is a unique technique that allows for
  the determination of velocity and a proxy for plasma density to be made
  throughout the corona and inner heliosphere (depending on observing
  frequency and distance observed from the Sun). Where sufficient
  observations are undertaken, the results are often used as input to
  space-weather forecast/prediction programmes and models as well as
  having a large scientific research value. By combining IPS results from
  multiple observing locations around the globe, we can increase both the
  temporal and spatial coverage across the whole of the inner heliosphere
  (and probe different coronal and heliospheric regions from near the Sun
  to beyond Earth's orbit). IPS also provides an excellent opportunity
  to enhance collaborations between developed and developing countries
  thanks to the locations of many of the IPS-capable systems currently
  in use or under development. There is now a defined IPS Common Data
  Format (IPSCDFv1.1) which is being implemented by the majority of the
  IPS community. <P />The Worldwide IPS Stations (WIPSS) Network aims to
  bring together, using IPSCDFv1.1, the worldwide real-time capable IPS
  observatories with well-developed and tested analyses techniques being
  unified across all single-site systems (such as MEXART, Pushchino,
  and Ooty) and cross-calibrated to the multi-site ISEE system (as
  well as learning from the scientific-based systems such as EISCAT,
  LOFAR, and the MWA). A WIPSS website is currently under development
  and has been showcased in late 2018 where updates are currently being
  implemented. An overview of the WIPSS Network will be presented, with
  some scientific highlights, along with progress to date and foreseen
  challenges (political, scientific, and financial) going forward.

---------------------------------------------------------
Title: Validating the Alfven Wave Solar Atmosphere (AWSoM) Model
    from the Low Corona to 1 AU
Authors: Sachdeva, N.; van der Holst, B.; Manchester, W.; Toth, G.;
   Lloveras, D. G.; Vásquez, A. M.; Lamy, P.; Jackson, B. V.; Henney,
   C. J.
2019AGUFMSH51A..04S    Altcode:
  The coronal/solar wind model, the Alfven Wave Solar atmosphere Model
  (AWSoM) a component within the Space Weather Modeling Framework (SWMF)
  follows a self-consistent physics-based global description of coronal
  heating and solar wind acceleration. AWSoM includes a description
  of low-frequency forward and counter-propagating Alfven waves that
  non-linearly interact resulting in a turbulent cascade and dissipative
  heating. In addition, there are separate temperatures for electrons and
  protons with collisional and collisionless heat conduction applied only
  to electrons and radiative losses based on the Chianti model. AWSoM
  extends from the base of the transition region where the strong
  density gradient necessitates self-consistent treatment of Alfven wave
  reflection and balanced turbulence. It includes a stochastic heating
  model as well as a description of proton parallel and perpendicular
  temperatures and kinetic instabilities based on temperature anisotropy
  and plasma beta.To validate AWSoM, we model Carrington rotations
  representative of solar minimum conditions and compare the simulation
  results with a comprehensive suite of observations. In the low corona
  (r &lt; 1.25 Rs), we compare with EUV images from both STEREOA/EUVI
  and SDO/AIA and to three-dimensional tomographic reconstructions of
  the electron temperature and density based on these same data. We
  also compare the model to tomographic reconstructions of the electron
  density from SOHO/LASCO observations (2.55 &lt; r &lt; 6 Rs). In
  the heliosphere, we compare model predictions of solar wind speed
  with velocity reconstructions from Interplanetary Scintillation
  observations. For comparison with observations near the Earth, we
  use OMNI data. Our results show that the AWSoM model performs well
  in quantitative agreement with the observations between the inner
  corona and 1 AU. In the lower corona, the model and the tomographic
  reconstructions agree within 20%-30% on average. The model also
  reproduces the fast solar wind speed in the polar regions. Near the
  Earth, our model shows good agreement with observations of solar wind
  velocity, electron temperature and density. The AWSoM model provides
  a comprehensive tool to study the solar corona and larger heliosphere
  with current and future solar missions as well as being well suited
  for space weather predictions.

---------------------------------------------------------
Title: Current Sheets, Magnetic Islands, and Associated Particle
    Acceleration in the Solar Wind as Observed by Ulysses near the
    Ecliptic Plane
Authors: Malandraki, Olga; Khabarova, Olga; Bruno, Roberto; Zank,
   Gary P.; Li, Gang; Jackson, Bernard; Bisi, Mario M.; Greco, Antonella;
   Pezzi, Oreste; Matthaeus, William; Chasapis Giannakopoulos, Alexandros;
   Servidio, Sergio; Malova, Helmi; Kislov, Roman; Effenberger, Frederic;
   le Roux, Jakobus; Chen, Yu; Hu, Qiang; Engelbrecht, N. Eugene
2019ApJ...881..116M    Altcode:
  Recent studies of particle acceleration in the heliosphere have
  revealed a new mechanism that can locally energize particles up to
  several MeV nucleon<SUP>-1</SUP>. Stream-stream interactions, as well
  as the heliospheric current sheet (CS)—stream interactions, lead to
  formation of large magnetic cavities, bordered by strong CSs, which in
  turn produce secondary CSs and dynamical small-scale magnetic islands
  (SMIs) of ∼0.01 au or less owing to magnetic reconnection. It has
  been shown that particle acceleration or reacceleration occurs via
  stochastic magnetic reconnection in dynamical SMIs confined inside
  magnetic cavities observed at 1 au. The study links the occurrence
  of CSs and SMIs with characteristics of intermittent turbulence and
  observations of energetic particles of keV-MeV nucleon<SUP>-1</SUP>
  energies at ∼5.3 au. We analyze selected samples of different
  plasmas observed by Ulysses during a widely discussed event, which was
  characterized by a series of high-speed streams of various origins that
  interacted beyond Earth’s orbit in 2005 January. The interactions
  formed complex conglomerates of merged interplanetary coronal
  mass ejections, stream/corotating interaction regions, and magnetic
  cavities. We study properties of turbulence and associated structures
  of various scales. We confirm the importance of intermittent turbulence
  and magnetic reconnection in modulating solar energetic particle flux
  and even local particle acceleration. Coherent structures, including
  CSs and SMIs, play a significant role in the development of secondary
  stochastic particle acceleration, which changes the observed energetic
  particle flux time-intensity profiles and increases the final energy
  level to which energetic particles can be accelerated in the solar wind.

---------------------------------------------------------
Title: The UCSD Iterative Tomography Interplanetary Scintillation
    (IPS) and In-situ Constraints on the ENLIL 3-D MHD Model
Authors: Jackson, Bernard V.; Odstrcil, Dusan; Hick, P. Paul;
   Buffington, Andrew; Tokumaru, Munetoshi; Bisi, Mario M.
2019shin.confE.120J    Altcode:
  The University of California, San Diego (UCSD) has developed a
  time-dependent three-dimensional (3-D) reconstruction technique that
  provides volumetric maps of density and velocity by constraining
  the ENLIL 3-D MHD model to fit interplanetary scintillation
  (IPS) observations and NOAA-provided in-situ plasma parameters
  at Earth in near real time. This system is compared with NOAA
  and NASA-provided in-situ measurements of plasma and fields and
  is now being evaluated for use in real time predictions of solar
  wind parameters a few days ahead of the present on the UCSD website
  https://ips.ucsd.edu/ENLIL_prediction. Unlike previous UCSD kinematic
  modeling, this new tomographic analysis with a 3-D MHD kernel now
  includes shock processes and the non-radial transport of structure
  from the inner-boundary source surface at 0.1 AU. Magnetic fields
  extrapolated outward from the solar surface support the iterative
  procedure, and are shown to provide a low-resolution several-day
  advance prediction of the background solar wind GSM Bz and geomagnetic
  storms. Used currently with IPS data available from ISEE, Japan,
  this type of programming will be especially important when more data
  become available from Worldwide IPS Stations (WIPSS) network groups
  and both spatial and temporal coverage is increased. Our modeling
  system complements existing operating systems at different world Space
  Weather Prediction Centers that currently use 3-D MHD modeling based
  primarily on magnetograms and NASA spacecraft imagery.

---------------------------------------------------------
Title: Validating the Alfven Wave Solar Model (AWSoM) from the lower
    corona to 1 AU
Authors: Sachdeva, Nishtha; Manchester, Ward; van der Holst, Bart;
   Toth, Gabor; Vasquez, Alberto; Jackson, Bernard; Lloveras, Diego G.;
   Mac Cormack, Cecilia; Yu, Hsiu-Shan
2019EGUGA..21.1465S    Altcode:
  We examine the steady state three-dimensional MHD simulations of the
  solar corona carried out with the new version of the Alfven Wave Solar
  Model (AWSoM) within the Space Weather Modeling framework (SWMF). AWSoM
  addresses the acceleration and heating of the solar corona via the
  interaction between counter-propagating Alfven waves. This non-linear
  interaction between the outward propagating low-frequency Alfven waves
  and those partially reflected by the speed gradients results in a
  turbulent energy cascade. The model uses physics-based partitioning
  of wave-dissipated heat between isotropic electron and anisotropic
  proton temperatures. To validate the AWSoM model, we select rotations
  representative of the solar minimum and maximum conditions and compare
  our simulation results with a comprehensive suite of observations. We
  use three-dimensional tomographic reconstructions of the electron
  temperature and density in the inner corona (r &lt; 1.25 Rsun) based
  on multi-wavelength extreme ultraviolet images from STEREO/EUVI
  and SDO/AIA. For comparison with observations made near the Earth,
  we compare the model with OMNI data. At different radial distances
  between 20 Rsun and 1 AU, we compare the model with reconstructions
  made with Interplanetary Scintillation (IPS) observations. Observations
  are compared with the simulated model results of plasma mass density,
  velocity, and magnetic fields, temperature anisotropy, and wave
  turbulence. Our results at solar minimum show that the improved AWSoM
  model performs well in agreement with the observations between inner
  corona and 1 AU. In the lower corona the model and the tomographic
  reconstructions match within a 20 % accuracy. Near the Earth, our model
  shows good agreement with observations of solar wind velocity, electron
  temperature and magnetic field. However, the electron density at 1 AU
  is overpredicted by the model for the solar minimum simulations. While
  this model version is already an improvement over previous predictions,
  we plan to validate our model using more Carrington rotations. The AWSoM
  model presents an extensive application to study the solar corona and
  larger heliosphere in concert with current and future solar missions.

---------------------------------------------------------
Title: Current State of Reduced Solar Activity: Intense Geomagnetic
    Storms
Authors: Manoharan, P. K.; Mahalakshmi, K.; Johri, A.; Jackson, B. V.;
   Ravikumar, D.; Kalyanasundaram, K.; Subramanian, S. P.; Mittal, A. K.
2018SunGe..13..135M    Altcode:
  We present a study of 21 geomagnetic storms, occurred during 2011-2017
  in association with the propagation of coronal mass ejections
  (CMEs). These storms are selected with the minimum storm disturbance
  index (SYM-H) intensity of -100 nT or less and are distributed from
  the maximum to the minimum of the weak solar cycle 24. We identify
  and investigate these storm-driving CMEs (halo and partial halo
  CMEs) by combining EUV and white-light images in the near-Sun region,
  interplanetary scintillation images in between the Sun and the Earth,
  and in-situ measurements at the near-Earth orbit. These CMEs cover
  a wide range of initial speeds, 180 to 2680 km/s. For about 50%
  of the CMEs, the fast initial speed at the near-Sun region does not
  correlate with the final speed at the near-Earth orbit. The storm
  indexes range between -100 and -233 nT and they are associated with
  minimum Bz values in the range of -12 to -38 nT. The Forbush decrease
  (FD) levels associated with these storms vary in the range of about -2%
  to -10%. A comparison of travel times of CMEs to 1 AU with the observed
  initial/final speeds and estimated initial speed suggests that a large
  fraction of fast initial speeds could possibly be due to the sudden
  expansion of the CME into a relatively low pressure interplanetary
  medium. Most of the geomagnetic storms (i.e., 19 storms) have been
  caused by the strong intrinsic magnetic field of the CME and only 2
  storms are produced by the sheath region between the arrival times of
  interplanetary shock and CME. The geomagnetic storm index is compared
  with the possible reconnection electric field component, BzVICME. It
  suggests an empirical relationship for the likely lower level of storm
  index, SYM-H = -70 - 0.003·BzVICME. (nT), in which Bz and VICME are
  respectively given in units of nT and km/s.

---------------------------------------------------------
Title: Tests of the UCSD Iterative Interplanetary Scintillation
    (IPS) Analysis Using Time-Dependent 3-D MHD Models as Kernels
Authors: Jackson, Bernard V.; Yu, Hsiu-Shan; Hick, P. Paul;
   Buffington, Andrew; Odstrcil, Dusan; Kim, Tae; Pogorelov, Nick;
   Tokumaru, Munetoshi; Bisi, Mario M.
2018shin.confE.193J    Altcode:
  The heliospheric group at the University of California, San Diego
  has developed a time-dependent three-dimensional (3-D) reconstruction
  technique which provides volumetric maps of density and velocity by
  iteratively fitting 3-D MHD models to interplanetary scintillation (IPS)
  observations. We have applied a similar technique in near real time to
  the IPS data for nearly 20 years. However, unlike the previous UCSD
  kinematic modeling, this new tomographic analysis now includes shock
  processes, as well as non-radial transport. Magnetic fields extrapolated
  outward from the solar surface, and in-situ spacecraft measurements near
  Earth can also be included to support the iterative procedure. Tests
  show that both CME and stream-interacting heliospheric density and
  velocity structures can be more accurately localized in extent relative
  to the previous kinematic analysis as structures move outward from the
  Sun. Shock sheath enhancements in front of high-speed heliospheric
  structures are also shown to be limited in extent by the iterative
  procedure. Examples of this analysis using ENLIL and the University
  of Alabama Multi-Scale Fluid-Kinetic Simulation Suite (MS-FLUKSS)
  heliospheric 3-D MHD codes as kernels will be shown. These examples
  can also refine poorly-known 3-D MHD variables (i.e., temperature), and
  parameters (gamma) by fitting heliospheric remotely-sensed structures
  near the solar surface, on their way through the heliosphere, and then
  later at 1 AU near Earth.

---------------------------------------------------------
Title: ASHI: An `All Sky' Heliospheric Imager for Viewing
    Thomson-Scattered Light
Authors: Jackson, Bernard; Hick, P.; Buffington, Andrew; Bisi, Mario
   M.; Yu, Hsiu-Shan; Edara, Jyothirmayi
2018cosp...42E1581J    Altcode:
  We have developed, and are now making a detailed design for an All-Sky
  Heliospheric Imager (ASHI), to fly on future deep-space missions. ASHI's
  principal long-term objective is acquisition of a precision photometric
  map of the inner heliosphere as viewed from deep space. Photometers on
  the twin Helios spacecraft, the Solar Mass Ejection Imager (SMEI) on
  the Coriolis satellite, and the Solar-TErrestrial RElations Observatory
  (STEREO) twin spacecraft Heliospheric Imagers (HIs), all indicate
  an optimum instrument design for visible-light Thomson-scattering
  observations. This design views a hemisphere of sky starting a few
  degrees from the Sun. Two imagers can cover almost all of the whole
  sky. A key photometric specification for ASHI is 0.1% differential
  photometry: this enables the three dimensional (3-D) reconstruction of
  density starting from near the Sun and extending outward. SMEI analyses
  have demonstrated the success of this technique, and when employed by
  ASHI, this will provide an order of magnitude better resolution in 3-D
  density over time. We augment this analysis to include remotely-sensed
  2-D velocity, and thus when these imagers are deployed in deep space
  they can provide comparisons of both imaged density and velocity to
  those measured in situ. We present recent progress in the instrument
  design, its expected performance specifications, and the possibilities
  for its deployment over the next few years.

---------------------------------------------------------
Title: Bz Determinations and Forecasts Using UCSD Analysis Techniques
Authors: Jackson, Bernard; Hick, P.; Buffington, Andrew; Yu, Hsiu-Shan;
   Zhao, Gary
2018cosp...42E1580J    Altcode:
  Since the middle of the last decade, UCSD has incorporated magnetic
  field data in its ISEE IPS tomographic analysis. These data are
  extrapolated upward from the solar surface using the Current Sheet
  Source Surface (CSSS) model (Zhao &amp; Hoeksema, 1995) provide
  predictions of the interplanetary field in RTN coordinates. When
  extrapolated to Earth, these fields can be displayed in a variety of
  ways, including GSM fields in Bx, By, and Bz coordinates. The Bz GSM
  field component gives a fair correlation with in-situ derived fields
  near Earth of a few nano-Tesla variation that maximizes in spring
  and fall as Russell and McPherron (1973) have shown, but even more
  significantly its daily variation is shown to be correlated with
  geomagnetic Kp and Dst indices. UCSD currently operates a website
  that predicts these transient low-resolution GSM Bz field component
  variations several days in advance. More challenging to predict are
  large, short-lived magnetic field components that can be north-south
  in RTN coordinates, and whose southward GSM Bz can provide the most
  extreme geomagnetic effects. Here, the record for success is not as
  clear, but there have been some inroads to these predictions from this
  analysis that will be discussed.

---------------------------------------------------------
Title: Tools for providing forecasts of Space Weather at the
    BepiColombo spacecraft pair during their forthcoming flybys of Venus
    and Mercury
Authors: McKenna-Lawlor, Susan; Jackson, Bernard; Odstrcil, Dusan
2018EGUGA..20.3334M    Altcode:
  The BepiColombo Mission to planet Mercury (launch 2018), will
  include during its Cruise Phase two flybys of Venus and five of
  Mercury. Its two constituent spacecraft (one provided by ESA - the
  Mercury Planetary Orbiter/MPO) and the other by JAXA - the Mercury
  Magnetospheric orbiter/MMO) will perform both autonomous and coordinated
  observations of the Venusian and Hermean environments during these flyby
  events. Two state of the art models/tools to predict the arrival of
  space weather at MPO and MMO during the flybys are presented. These
  tools comprise theInterplanetary Scintillation 3D-reconstruction
  Technique (IPS analyses) which was developed in time-dependent form at
  the University of California, San Diego to provide precise tomographic
  3D-reconstructions of the, time-varying, global heliosphere. The
  other tool ENLIL is a time-dependent 3-D MHD model of the heliosphere
  which solves equations for: plasma mass; momentum; energy density; and
  magnetic field; using a Flux-Corrected-Transport (FCT) algorithm. It
  has already been demonstrated by the authors (PSS, 2017) that the
  above mentioned tools are individually appropriate to predict the
  arrival of space weather at the BepiColombo spacecraft pair during
  their forthcoming Venus flybys. A new algorithm has recently been
  developed which melds ENLIL with IPS, thereby allowing an iterative use
  of IPS data to update and fit the modelling by ENLIL of heliospheric
  structures. This methodology is presented in the present paper and used
  to retrospectively predict the arrival of solar disturbances at the
  Mercury Messenger spacecraft during its mission period 2011-2015. The
  method is demonstrated to yield higher time resolution in providing
  space weather predictions at BepiColombo during its flybys of Mercury
  than is obtained using either ENLIL or IPS alone since it can link
  observations made in-situ with those observed remotely. The time in
  advance of the flybys planned to be utilized by the Operations Team for
  uploading commands/information to the spacecraft is very long. Thus,
  switching-on or switching-off of the payload instruments in advance
  of significant solar events is presently not feasible. This could
  result in its only being possible to use the predictions to select
  those measurements for downloading inferred to importantly illustrate
  the interaction of Mercury with the disturbed solar wind. Analysis of
  these data would then be implemented on the ground.

---------------------------------------------------------
Title: Interplanetary Scintillation with the Murchison Widefield Array
I: a sub-arcsecond survey over 900 deg<SUP>2</SUP> at 79 and 158 MHz
Authors: Morgan, J. S.; Macquart, J. -P.; Ekers, R.; Chhetri, R.;
   Tokumaru, M.; Manoharan, P. K.; Tremblay, S.; Bisi, M. M.; Jackson,
   B. V.
2018MNRAS.473.2965M    Altcode: 2017arXiv170900312M
  We present the first dedicated observations of Interplanetary
  Scintillation (IPS) with the Murchison Widefield Array. We have
  developed a synthesis imaging technique, tailored to the properties
  of modern 'large-N' low-frequency radio telescopes. This allows us to
  image the variability on IPS time-scales across 900 deg<SUP>2</SUP>
  simultaneously. We show that for our observations, a sampling
  rate of just 2 Hz is sufficient to resolve the IPS signature of
  most sources. We develop tests to ensure that IPS variability is
  separated from ionospheric or instrumental variability. We validate
  our results by comparison with existing catalogues of IPS sources,
  and near-contemporaneous observations by other IPS facilities. Using
  just 5 min of data, we produce catalogues at both 79 and 158 MHz,
  each containing over 350 scintillating sources. At the field centre,
  we detect approximately one scintillating source per square degree,
  with a minimum scintillating flux density at 158 MHz of 110 mJy,
  corresponding to a compact flux density of approximately 400 mJy. Each
  of these sources is a known radio source, however only a minority
  were previously known to contain sub-arcsecond components. We discuss
  our findings and the prospects they hold for future astrophysical and
  heliospheric studies.

---------------------------------------------------------
Title: The Worldwide Interplanetary Scintillation (IPS) Stations
(WIPSS) Network October 2016 Observing Campaign: Initial WIPSS
    Data Analyses
Authors: Bisi, M. M.; Fallows, R. A.; Jackson, B. V.; Tokumaru, M.;
   Gonzalez-Esparza, A.; Morgan, J.; Chashei, I. V.; Mejia-Ambriz, J.;
   Tyul'bashev, S. A.; Manoharan, P. K.; De la Luz, V.; Aguilar-Rodriguez,
   E.; Yu, H. S.; Barnes, D.; Chang, O.; Odstrcil, D.; Fujiki, K.;
   Shishov, V.
2017AGUFMSH21A2648B    Altcode:
  Interplanetary Scintillation (IPS) allows for the determination of
  velocity and a proxy for plasma density to be made throughout the corona
  and inner heliosphere. Where sufficient observations are undertaken,
  the results can be used as input to the University of California,
  San Diego (UCSD) three-dimensional (3-D) time-dependent tomography
  suite to allow for the full 3-D reconstruction of both velocity and
  density throughout the inner heliosphere. By combining IPS results
  from multiple observing locations around the planet, we can increase
  both the temporal and spatial coverage across the whole of the inner
  heliosphere and hence improve forecast capability. During October 2016,
  a unique opportunity arose whereby the European-based LOw Frequency
  ARray (LOFAR) radio telescope was used to make nearly four weeks of
  continuous observations of IPS as a heliospheric space-weather trial
  campaign. This was expanded into a global effort to include observations
  of IPS from the Murchison Widefield Array (MWA) in Western Australia
  and many more observations from various IPS-dedicated WIPSS Network
  systems. LOFAR is a next-generation low-frequency radio interferometer
  capable of observing in the radio frequency range 10-250 MHz, nominally
  with up to 80 MHz bandwidth at a time. MWA in Western Australia is
  capable of observing in the 80-300 MHz frequency range nominally using
  up to 32 MHz of bandwidth. IPS data from LOFAR, ISEE, the MEXican Array
  Radio Telescope (MEXART), and, where possible, other WIPSS Network
  systems (such as LPI-BSA and Ooty), will be used in this study and we
  will present some initial findings for these data sets. We also make
  a first attempt at the 3-D reconstruction of multiple pertinent WIPSS
  results in the UCSD tomography. We will also try to highlight some
  of the potential future tools that make LOFAR a very unique system to
  be able to test and validate a whole plethora of IPS analysis methods
  with the same set of IPS data.

---------------------------------------------------------
Title: ASHI: An All Sky Heliospheric Imager for Viewing
    Thomson-Scattered Light
Authors: Buffington, A.; Jackson, B. V.; Yu, H. S.; Hick, P. P.;
   Bisi, M. M.
2017AGUFMSH23D2689B    Altcode:
  We have developed, and are now making a detailed design for an All-Sky
  Heliospheric Imager (ASHI), to fly on future deep-space missions. ASHI's
  principal long-term objective is acquisition of a precision photometric
  map of the inner heliosphere as viewed from deep space. Photometers
  on the twin Helios spacecraft, the Solar Mass Ejection Imager
  (SMEI) upon the Coriolis satellite, and the Heliospheric Imagers
  (HIs) upon the Solar-TErrestrial RElations Observatory (STEREO)
  twin spacecraft, all indicate an optimum instrument design for
  visible-light Thomson-scattering observations. This design views a
  hemisphere of sky starting a few degrees from the Sun. Two imagers can
  cover almost all of the whole sky. A key photometric specification
  for ASHI is 0.1% differential photometry: this enables the three
  dimensional reconstruction of density starting from near the Sun
  and extending outward. SMEI analyses have demonstrated the success
  of this technique: when employed by ASHI, this will provide an order
  of magnitude better resolution in 3-D density over time. We augment
  this analysis to include velocity, and these imagers deployed in deep
  space can thus provide high-resolution comparisons both of direct
  in-situ density and velocity measurements to remote observations of
  solar wind structures. In practice we find that the 3-D velocity
  determinations provide the best tomographic timing depiction of
  heliospheric structures. We discuss the simple concept behind this,
  and present recent progress in the instrument design, and its expected
  performance specifications. A preliminary balloon flight of an ASHI
  prototype is planned to take place next Summer.

---------------------------------------------------------
Title: The variable nature of the solar wind
Authors: Jackson, B. V.; Yu, H. S.; Buffington, A.; Hick, P. P.
2017AGUFMSH23D2684J    Altcode:
  When analyzing LASCO C2 and STEREO SECCHI COR2 coronagraph images,
  and using UCSD-developed two-dimensional (2D) correlation-tracking
  techniques, we found that the observed outflow is not a static
  well-ordered motion, but instead has highly variable speed
  structures. This outward motion of structures is also observed over
  the entire high-resolution STEREO HI-1 field of view, whether or not
  a CME is present. We have recently exploited the correlation-tracking
  techniques to measure the optical flow on HI-1A images. The analysis
  yields a wealth of information about the outward motion of large-
  and fine-scale structures in the heliosphere. These include the 2D
  speed of features, the level of the correlation, the brightness of
  the feature measured, and the structure non-radial 2D motion. Here
  we present the analysis of a well-observed fast-moving CME and the
  speed of different structures within it. The preliminary results of
  the heliospheric velocity determination using HI-1A images show the
  nature of the solar wind within the CME that is organized into a fast
  and patchy high-speed front followed by a slower internal region. From
  this we conclude that the Parker Solar Probe and ESA Solar Orbiter
  will measure this highly-variable structure in situ within CMEs,
  and we speculate that these structures will also show abundance and
  magnetic field differences related to this high variability.

---------------------------------------------------------
Title: An Iterative Interplanetary Scintillation (IPS) Analysis
    Using Time-dependent 3-D MHD Models as Kernels
Authors: Jackson, B. V.; Yu, H. S.; Hick, P. P.; Buffington, A.;
   Odstrcil, D.; Kim, T. K.; Pogorelov, N. V.; Tokumaru, M.; Bisi, M. M.;
   Kim, J.; Yun, J.
2017AGUFMSH21A2650J    Altcode:
  The University of California, San Diego has developed an iterative
  remote-sensing time-dependent three-dimensional (3-D) reconstruction
  technique which provides volumetric maps of density, velocity, and
  magnetic field. We have applied this technique in near real time for
  over 15 years with a kinematic model approximation to fit data from
  ground-based interplanetary scintillation (IPS) observations. Our
  modeling concept extends volumetric data from an inner boundary placed
  above the Alfvén surface out to the inner heliosphere. We now use this
  technique to drive 3-D MHD models at their inner boundary and generate
  output 3-D data files that are fit to remotely-sensed observations
  (in this case IPS observations), and iterated. These analyses are
  also iteratively fit to in-situ spacecraft measurements near Earth. To
  facilitate this process, we have developed a traceback from input 3-D
  MHD volumes to yield an updated boundary in density, temperature,
  and velocity, which also includes magnetic-field components. Here
  we will show examples of this analysis using the ENLIL 3D-MHD and
  the University of Alabama Multi-Scale Fluid-Kinetic Simulation Suite
  (MS-FLUKSS) heliospheric codes. These examples help refine poorly-known
  3-D MHD variables (i.e., density, temperature), and parameters (gamma)
  by fitting heliospheric remotely-sensed data between the region near
  the solar surface and in-situ measurements near Earth.

---------------------------------------------------------
Title: 3D-MHD Modeling Fit to Interplanetary Scintillation (IPS)
    Observations
Authors: Jackson, Bernard Vernon; Yu, Hsiu-Shan; Hick, P. Paul;
   Buffington, Andrew; Bisi, Mario M.; Odstrcil, Dusan; Kim, Tae;
   Pogorelov, Nick; Tokumaru, Munetoshi; Kim, Jaehun; Yun, Jongyeon
2017shin.confE.125J    Altcode:
  The University of California, San Diego has developed an iterative
  remote-sensing time-dependent three-dimensional (3D) reconstruction
  technique which provides volumetric maps of density, velocity, and
  magnetic field. We have applied this technique in near real time for
  over 15 years with a kinematic model approximation to fit data from
  ground-based interplanetary scintillation (IPS) observations. Our
  modeling concept extends volumetric data from an inner boundary placed
  above the Alfvén surface out to the inner heliosphere. We now use this
  technique to drive 3D-MHD models at their inner boundary and generate
  output 3D data files that are fit to remotely-sensed observations (in
  this case IPS observations), and iterated. These analyses are also
  iteratively fit to in-situ spacecraft measurements near Earth. To
  facilitate this process, we have developed a traceback from input
  3D-MHD volumes to yield an updated boundary in density, temperature,
  and velocity, which also includes magnetic-field components. Here
  we will show examples of this analysis using the ENLIL 3D-MHD and
  the University of Alabama Multi-Scale Fluid-Kinetic Simulation Suite
  (MS-FLUKSS) heliospheric codes.

---------------------------------------------------------
Title: Observations and Analyses of Heliospheric Faraday Rotation of
    a Coronal Mass Ejection (CME) Using the LOw Frequency ARray (LOFAR)
    and Space-Based Imaging Techniques
Authors: Bisi, Mario Mark; Jensen, Elizabeth; Sobey, Charlotte;
   Fallows, Richard; Jackson, Bernard; Barnes, David; Giunta, Alessandra;
   Hick, Paul; Eftekhari, Tarraneh; Yu, Hsiu-Shan; Odstrcil, Dusan;
   Tokumaru, Munetoshi; Wood, Brian
2017EGUGA..1913243B    Altcode:
  Geomagnetic storms of the highest intensity are general driven
  by coronal mass ejections (CMEs) impacting the Earth's space
  environment. Their intensity is driven by the speed, density, and,
  most-importantly, their magnetic-field orientation and magnitude
  of the incoming solar plasma. The most-significant magnetic-field
  factor is the North-South component (Bz in Geocentric Solar Magnetic
  - GSM - coordinates). At present, there are no reliable prediction
  methods available for this magnetic-field component ahead of the
  in-situ monitors around the Sun-Earth L1 point. Observations of Faraday
  rotation (FR) can be used to attempt to determine average magnetic-field
  orientations in the inner heliosphere. Such a technique has already
  been well demonstrated through the corona, ionosphere, and also the
  interstellar medium. Measurements of the polarisation of astronomical
  (or spacecraft in superior conjunction) radio sources (beacons/radio
  frequency carriers) through the inner corona of the Sun to obtain
  the FR have been demonstrated but mostly at relatively-high radio
  frequencies. Here we show some initial results of true heliospheric FR
  using the Low Frequency Array (LOFAR) below 200 MHz to investigate
  the passage of a coronal mass ejection (CME) across the line of
  sight. LOFAR is a next-generation low-frequency radio interferometer,
  and a pathfinder to the Square Kilometre Array (SKA) - LOW telescope. We
  demonstrate preliminary heliospheric FR results through the analysis of
  observations of pulsar J1022+1001, which commenced on 13 August 2014 at
  13:00UT and spanned over 150 minutes in duration. We also show initial
  comparisons to the FR results via various modelling techniques and
  additional context information to understand the structure of the inner
  heliosphere being detected. This observation could indeed pave the way
  to an experiment which might be implemented for space-weather purposes
  that will eventually lead to a near-global method for determining the
  magnetic field throughout the inner heliosphere.

---------------------------------------------------------
Title: Atypical energetic particle events observed prior energetic
    particle enhancements associated with corotating interaction regions
Authors: Khabarova, Olga; Malandraki, Olga; Zank, Gary; Jackson,
   Bernard; Bisi, Mario; Desai, Mihir; Li, Gang; le Roux, Jakobus;
   Yu, Hsiu-Shan
2017EGUGA..1910358K    Altcode:
  Recent studies of mechanisms of particle acceleration in the
  heliosphere have revealed the importance of the comprehensive analysis
  of stream-stream interactions as well as the heliospheric current
  sheet (HCS) - stream interactions that often occur in the solar wind,
  producing huge magnetic cavities bounded by strong current sheets. Such
  cavities are usually filled with small-scale magnetic islands
  that trap and re-accelerate energetic particles (Zank et al. ApJ,
  2014, 2015; le Roux et al. ApJ, 2015, 2016; Khabarova et al. ApJ,
  2015, 2016). Crossings of these regions are associated with unusual
  variations in the energetic particle flux up to several MeV/nuc near
  the Earth's orbit. These energetic particle flux enhancements called
  "atypical energetic particle events" (AEPEs) are not associated
  with standard mechanisms of particle acceleration. The analysis of
  multi-spacecraft measurements of energetic particle flux, plasma
  and the interplanetary magnetic field shows that AEPEs have a local
  origin as they are observed by different spacecraft with a time delay
  corresponding to the solar wind propagation from one spacecraft to
  another, which is a signature of local particle acceleration in the
  region embedded in expanding and rotating background solar wind. AEPEs
  are often observed before the arrival of corotating interaction
  regions (CIRs) or stream interaction regions (SIRs) to the Earth's
  orbit. When fast solar wind streams catch up with slow solar wind,
  SIRs of compressed heated plasma or more regular CIRs are created
  at the leading edge of the high-speed stream. Since coronal holes
  are often long-lived structures, the same CIR re-appears often for
  several consecutive solar rotations. At low heliographic latitudes,
  such CIRs are typically bounded by forward and reverse waves on their
  leading and trailing edges, respectively, that steepen into shocks at
  heliocentric distances beyond 1 AU. Energetic ion increases have been
  frequently observed in association with CIR's shocks, and these shocks
  to be believed to accelerate ions up to several MeV per nucleon. In this
  paradigm particle acceleration is commonly believed to occur mainly at
  the well-formed reverse shock at 2-3 AU with particles streaming back
  from the shocks from the outer heliosphere to 1 AU (Malandraki et al.,
  2007). However, AEPEs observed for many hours before the crossing of
  the forward shock (or even before the leading edge of a CIR without
  well-formed forward shock) cannot be explained within the framework
  of this paradigm. We have recently found that the effect of pre-CIR
  AEPEs occurs mainly as a result of the formation of a region filled
  with magnetic islands compressed between the high-density leading edge
  of a CIR and the HCS (Khabarova et al. ApJ, 2016). We show here that
  any kind of complicated stream-CIR interactions may lead to the same
  effect due to the formation of magnetic cavities in front of CIRs. The
  analysis of in situ multi-spacecraft measurements often suggests very
  complicated ways of propagation of streams and current sheets that form
  magnetic cavities. In the case of multiple stream-stream interaction,
  comparisons of data from distant spacecraft may be puzzling and even
  useless for understanding the large-scale topology of the region of
  particle acceleration, because even several point measurements cannot
  reconstruct approximate forms of the magnetic cavities and shed light on
  the pre-history of their origin and evolution. We employ interplanetary
  scintillation tomographic data for reconstructions of the solar wind
  speed, density and interplanetary magnetic field profiles to understand
  a 3-D picture of stream interactions responsible for pre-CIR AEPEs. This
  project has received funding from the European Union's Horizon 2020
  research and innovation programme under grant agreement No 637324

---------------------------------------------------------
Title: Modeling the Solar Wind throughout Interplanetary Space Using
    Ground-based and Spacecraft Observational Data
Authors: Kim, T. K.; Pogorelov, N. V.; Arge, C. N.; Elliott, H. A.;
   Jackson, B. V.; Kryukov, I.; Manoharan, P. K.; McComas, D. J.; Yu,
   H. S.; Zank, G. P.
2016AGUFMSM32A..03K    Altcode:
  The solar wind is a turbulent medium with physical properties
  fluctuating on multiple scales. We model the three-dimensional,
  time-dependent solar wind plasma flow using our own software Multi-Scale
  Fluid-Kinetic Simulation Suite (MS-FLUKSS), which, in addition to the
  thermal solar wind plasma, takes into account charge exchange of solar
  wind protons with interstellar neutral atoms and treats nonthermal
  ions (i.e., pickup ions) born during this process as a separate
  fluid. Additionally, MS-FLUKSS allows us to model turbulence generated
  by pickup ions. Using adaptive mesh refinement, we can efficiently
  model propagation of sophisticated structures such as coronal mass
  ejections at high resolution. As part of our long-term goal to build
  realistic time-dependent solar wind models capable of reproducing the
  plasma flow, magnetic field, and turbulence throughout the heliosphere,
  we have been experimenting with time-dependent boundary conditions
  derived from remote-sensing observations (e.g., interplanetary
  scintillation) of the solar wind and also from empirically-driven
  coronal model outputs. We report on the progress of these modeling
  efforts. In a more focused study, we used MS-FLUKSS to investigate the
  evolution of plasma and turbulent fluctuations along the trajectory
  of the New Horizons spacecraft using plasma and turbulence parameters
  from OMNI data as time-dependent boundary conditions at 1 AU for the
  Reynolds-averaged MHD equations. We compare this model with in situ
  plasma observations by New Horizons.

---------------------------------------------------------
Title: Interplanetary Scintillation Observations with a New Generation
of Radio Telescopes: First results from the MWA
Authors: Morgan, J. S.; Macquart, J. P.; Ekers, R.; Bisi, M. M.;
   Jackson, B. V.; Tokumaru, M.; Manoharan, P. K.; Chhetri, R.
2016AGUFMSH22B..05M    Altcode:
  Interplanetary scintillation (IPS) is a phenomenon which can be used
  to probe both the heliospheric plasma and the structure of compact
  astrophysical radio sources. It is a vital tool for near-real-time
  monitoring of space weather. Previous IPS studies have generally
  relied on single concentrated collecting areas (either phased arrays
  or dishes). The Murchison Widefield Array (MWA) by contrast is a
  new-generation instrument consisting of a 128-element interferometer
  with an extremely wide field of view, and outstanding instantaneous
  imaging capability. This enables IPS studies of 1000 sources
  simultaneously, increasing the number of daily measurements that
  can be made by a factor of two or more. Here we report on progress
  from an ongoing IPS survey with the MWA where observations are made
  simultaneously at 80MHz and 150MHz. Dual-frequency observations allow
  solar wind velocities to be determined even with a single station,
  more accurately than from the analyses of a single-frequency IPS
  spectrum alone. Furthermore, the different refractive indices at
  different wavelengths leads to a lag in the cross correlation of the
  two frequency bands. This allows the bulk density of the outer solar
  corona to be probed along multiple lines of sight. We will discuss
  recent results and how they might be integrated into international
  Space Weather Prediction efforts such as the Worldwide IPS Stations
  (WIPSS) Network.

---------------------------------------------------------
Title: Observations of Heliospheric Faraday Rotation of a CME Using
    LOFAR and Space-Based Imaging
Authors: Bisi, M. M.; Jensen, P. E., E. A.; Sobey, C.; Fallows, R. A.;
   Jackson, B. V.; Barnes, D.; Giunta, A. S.; Hick, P. P.; Eftekhari,
   T.; Yu, H. S.; Odstrcil, D.; Tokumaru, M.; Wood, B. E.
2016AGUFMSH11C2251B    Altcode:
  The most-intense space weather at Earth consists of geomagnetic
  storms where their intensity is driven by the speed, density,
  and magnetic-field orientation of the incoming solar plasma. The
  most-significant factor is the North-South component of magnetic field
  (Bz in Geocentric Solar Magnetic - GSM - coordinates). At present,
  there is no reliable prediction of this magnetic-field component ahead
  of the in-situ monitors around the Sun-Earth L1 point. Observations
  of Faraday rotation (FR) can be used to attempt to determine average
  magnetic-field orientations in the inner heliosphere, a technique which
  has already been well demonstrated through the corona, ionosphere, and
  interstellar medium. Measurements of the polarization of astronomical
  (or spacecraft in superior conjunction) radio sources (beacons/radio
  frequency carriers) through the inner corona of the Sun to obtain
  the FR have been demonstrated but mostly at relatively-high radio
  frequencies. Here we show some initial results of true heliospheric FR
  using the Low Frequency Array (LOFAR) below 200 MHz to investigate
  the passage of a coronal mass ejection (CME) across the line of
  sight. LOFAR is a next-generation low-frequency radio interferometer,
  and a pathfinder to the Square Kilometre Array (SKA) - LOW telescope. We
  demonstrate preliminary heliospheric FR results through the analysis
  of observations of pulsar J1022+1001, which commenced on 13 August
  2014 at 13:00UT and spanned over 150 minutes in duration. We also show
  initial comparisons to the FR results via various modelling techniques
  and additional context information to understand the structure of the
  inner heliosphere being detected. This observation could pave the way
  to an experiment which might be implemented for space-weather purposes
  that will eventually lead to a near-global method for determining the
  magnetic field throughout the inner heliosphere.

---------------------------------------------------------
Title: Potential Use of Observations of Interplanetary Scintillation
    (IPS) and Faraday Rotation (FR) in Support of the Solar Orbiter and
    Solar Probe Plus Missions
Authors: Bisi, M. M.; Giunta, A. S.; Jensen, P. E., E. A.;
   Jackson, B. V.; Fallows, R. A.; Chang, O.; Gonzalez-Esparza, A.;
   Aguilar-Rodriguez, E.; Barnes, D.; Tokumaru, M.; Manoharan, P. K.;
   Odstrcil, D.; Yu, H. S.; Wexler, D.
2016AGUFMSH53A..09B    Altcode:
  The Solar Orbiter (SO) and Solar Probe Plus (SPP) spacecraft (both
  due to be launched in 2018) are missions intended to have close
  encounters with the Sun. Their overarching goals are to investigate
  the Sun-heliosphere connections by remotely-sensing and/or directly
  sampling the near-Sun coronal and inner-heliosphere plasma and by
  flying closer-in to the Sun than any previous mission (with the
  exception of MESSENGER and Helios). In particular, SPP will fly deep
  into the solar corona reaching 10 solar radii at its closest orbital
  perihelion. Such complex missions will only be undertaking full
  science in bursts due to telemetry constraints and abilities to make
  contact with the spacecraft and thus much forward planning is needed,
  especially for SO. Therefore, both missions will strongly benefit
  from long-term context information for the observational planning
  stages and connection science, using other spacecraft further out
  from the Sun that may be still in operation (e.g. STEREO-A, SOHO,
  DSCOVR, etc…) as well as ground-based observations from Earth. The
  techniques of interplanetary scintillation (IPS) and Faraday rotation
  (FR), applied to the corona, and the inner heliosphere, can provide
  additional global and local context information in the form of several
  plasma parameters related to the velocity, density, and magnetic field,
  especially via tomographic/modelling combinations. Here, we highlight
  to the wider communities some of these capabilities and potential for
  context provision as well as joint science opportunities (particularly
  at higher-frequency IPS and inner-coronal FR) ahead of the two missions
  being launched.

---------------------------------------------------------
Title: Observations of the Variable Coronal Solar Wind, and its
    Implications for Solar Probe Plus and Solar Orbiter
Authors: Jackson, B. V.; Yu, H. S.; Hick, P. P.; Buffington, A.
2016AGUFMSH43B2565J    Altcode:
  Solar wind observations from Ulysses show polar solar regions at solar
  minimum to be uniform and non-structured. However, when analyzing LASCO
  C2 and STEREO SECCHI COR2 coronagraph images, and using UCSD-developed
  correlation-tracking techniques, we find the observed solar wind
  outflow during these periods is not a static well-ordered motion,
  but instead has highly-variable speed structures. These high-speed
  polar structures are associated with slightly brighter (and also
  patchy) coronal structures. When the high-speed patches are averaged
  with the slower surrounding corona, the solar wind acceleration with
  solar distance is observed consistently across the polar coronal hole
  regions. This change in speed with distance is also consistent with
  the outward flow speed observed in polar regions determined from mass
  flux considerations and known coronagraph polarization brightness. From
  this we conclude that Solar Probe Plus and Solar Orbiter will not only
  be able to measure these structures in situ as variable wind, but they
  may also be able to determine the key parameters associated with these
  structures and how these parameters (abundances and magnetic fields)
  are related to the solar wind acceleration that is observed remotely
  in coronagraph observations.

---------------------------------------------------------
Title: ASHI, an All Sky Heliospheric Imager for Future NASA Missions
Authors: Jackson, B. V.; Buffington, A.; Hick, P. P.; Yu, H. S.;
   Bisi, M. M.
2016AGUFMSH11C2276J    Altcode:
  We wish to answer the scientific question: "What are the shapes and time
  histories of heliospheric structures in the plasma parameters, density
  and velocity as structures move outward from the Sun and surround the
  spacecraft?" To provide answers to this question, we propose ASHI,
  an All-Sky Heliospheric Imager for future NASA missions. ASHI's
  primary applicability is to view the inner heliosphere from deep
  space as a photometric system. The zodiacal-light photometers
  on the twin Helios spacecraft, the Solar Mass Ejection Imager
  (SMEI) on the Coriolis satellite, and the Heliospheric Imagers
  (HIs) on the Solar-TErrestrial RElations Observatory (STEREO) twin
  spacecraft, all point the way towards an optimum instrument for viewing
  Thomson-scattering observations. The specifications for such systems
  include viewing the whole sky starting beyond a few degrees of the Sun,
  and covering a hemisphere or more of sky. With an imager mass of about
  2.5 kg per system (scalable to lower values for instruments viewing
  from closer than 1 AU), ten-minute exposures, 20 arc-second pointing,
  and low power consumption, this type of instrument has been a popular
  choice for recent NASA Mission concepts such as STEREO, Solar Orbiter,
  Solar probe, and EASCO. A key photometric specification for such imagers
  is 0.1% differential photometry which enables the 3-D reconstruction
  of density starting from near the Sun and extending outward. A proven
  concept using SMEI analyses, ASHI will provide an order of magnitude
  better resolution in three dimensions over time. As a new item we intend
  to include velocity in this concept, and for a heliospheric imager in
  deep space, provide high-resolution comparisions of in-situ density
  and velocity measurements obtained at the spacecraft, to structures
  observed remotely.

---------------------------------------------------------
Title: The UCSD Time-dependent Tomography and IPS use for Exploring
    Space Weather Events
Authors: Yu, H. S.; Jackson, B. V.; Buffington, A.; Hick, P. P.;
   Tokumaru, M.; Odstrcil, D.; Kim, J.; Yun, J.
2016AGUFMSH22B..06Y    Altcode:
  The University of California, San Diego (UCSD) time-dependent,
  iterative, kinematic reconstruction technique has been used and expanded
  upon for over two decades. It provides some of the most-accurate
  predictions and three-dimensional (3D) analyses of heliospheric
  solar-wind parameters now available using interplanetary scintillation
  (IPS) data. The parameters provided include reconstructions of
  velocity, density, and three-component magnetic fields. Precise
  time-dependent results are now obtained at any solar distance in the
  inner heliosphere using ISEE (formerly STELab), Japan, IPS data sets,
  and can be used to drive 3D-MHD models including ENLIL. Using IPS
  data, these reconstructions provide a real-time prediction of the
  global solar wind parameters across the whole heliosphere with a time
  cadence of about one day (see http://ips.ucsd.edu). Here we compare
  the results (such as density, velocity, and magnetic fields) from the
  IPS tomography with different in-situ measurements and discuss several
  specific space weather events that demonstrate the issues resulting
  from these analyses.

---------------------------------------------------------
Title: Determination of magnetic-field components from inner-corona
    closed-loop propagation and IPS analysis
Authors: Jackson, Bernard; Tokumaru, Munetoshi; Gonzalez-Esparza,
   Americo; Hick, P.; Buffington, Andrew; Hong, Sunhak; Bisi, Mario M.;
   Kim, Jaehun; Yu, Hsiu-Shan
2016cosp...41E.882J    Altcode:
  We find that a portion of the interplanetary magnetic field measured
  in situ near Earth is present from a direct outward mapping of closed
  fields from the low solar corona. The Current-Sheet Source Surface
  (CSSS) model (Zhao &amp; Hoeksema, 1995 JGR 100, 19), extrapolate
  magnetogram-derived fields upward from near the solar surface. Global
  velocities and densities inferred from a combination of observations
  of interplanetary scintillation (IPS), matched to in-situ velocities
  and densities measured by spacecraft instrumentation, then provide an
  accurate outward timing to 1 AU using the UCSD tomography model that
  assumes conservation of mass and mass flux. All three field components
  at 1 AU are present including the north-south (or Bn) component field,
  and are compared with the appropriate ACE magnetometer in-situ (RTN)
  field coordinate. A significant positive daily correlation variation
  sometimes as high as 0.8 exists between these closed loop components
  and those determined by in-situ measurement over the last ten years
  for individual Carrington rotations. We determine that a consistent
  small fraction of the static low-coronal component flux (∼2%),
  that includes the Bn component, regularly escapes from closed-field
  regions. However, this percentage of closed projected fields relative
  to those measured in situ at Earth varies somewhat, indicating that a
  more efficient process for this flux propagation exists at the peak of
  the solar cycle than at its minimum. Since the Bn field provides the
  major portion of the Geocentric Solar Magnetospheric (GSM) Bz field
  component that couples most closely to the Earth's geomagnetic field,
  the prospects of using this technique for space weather predictions
  are being actively developed.

---------------------------------------------------------
Title: Incorporation of MEXART Interplanetary Scintillation (IPS) Data
    into the UCSD 3-D Tomography as Part of the Worldwide IPS Stations
(WIPSS) Initiative: Enhancing Space Weather Science and Forecasting
Authors: Chang, Oyuki; Jackson, Bernard V.; González-Esparza, Americo;
   Yu, Hsiu-Shan; Mejia-Ambriz, Julio
2016shin.confE..35C    Altcode:
  The University of California, San Diego has developed a 3-D tomography
  reconstruction program that employs kinematic solar wind model. It uses
  IPS data to reconstruct heliospheric solar wind velocity and density,
  and extrapolates magnetic field outward from the solar surface using
  the IPS velocities. Results from the 3-D tomography have been obtained
  in the past from ISEE (formerly STELab), Japan IPS data sets, but the
  technique can also incorporate data from other IPS stations around
  the world that use a 'standard' IPS format. The MEXican Array Radio
  Telescope (MEXART) is the only radio array dedicated to IPS observations
  in the Americas and has an operating frequency of 140 MHz. We have
  employed the IPS data set from MEXART to calibrate and incorporate it
  into the 3-D tomography, and in this way we can integrate MEXART data
  sets and data from other instruments like Big Scanning Array (BSA)
  in Pushchino, Russia in order to generate more accurate predictions
  and 3-D reconstructions as part of the Worldwide IPS Stations (WIPSS)
  Initiative.

---------------------------------------------------------
Title: The 2014 August 19 CME VarSITI ISEST Event Observed in ISEE
    IPS Observations with the UCSD Time-dependent Tomography
Authors: YU, HSIU-SHAN; Jackson, B. V.; Buffington, A.; Hick, P. P.;
   Chang, O.; Tokumaru, M.
2016shin.confE..28Y    Altcode:
  The 2014 August 19 CME shows a large in-situ density response at
  Earth, and is a well-observed event in Institute for Space-Earth
  Environmental Research (ISEE), Japan, interplanetary scintillation
  (IPS) analyses. This event is documented as a case-study example of
  the many events that can be reconstructed and viewed in 3D, with time
  extending from first measurements in coronagraph observations to their
  in-situ manifestation at Earth. Here, as usual, we find that the UCSD
  tomography IPS-reconstructed g-level images for this event have nearly
  the same structure as was observed in coronagraph images three days
  earlier, before the CME arrived at Earth. The density enhancement that
  arrives at Earth is well-reproduced in Advanced Composition Explorer
  (ACE) and Charge, Element and Isotope Analysis System (CELIAS) in-situ
  data; the differences between these data sets and those from Wind
  are shown. Although this is a slow event, and thus very well-observed
  using only the ISEE radio observatory data, this study indicates how
  a network of IPS sites around the world could also map the fastest
  Earth-directed CMEs.

---------------------------------------------------------
Title: Preliminary Analysis of Observations of Heliospheric Faraday
    Rotation of a CME Using LOFAR
Authors: Bisi, Mario M.; Jensen, Elizabeth A.; Sobey, Charlotte;
   Fallows, Richard A.; Jackson, Bernard V.; Barnes, David; Giunta,
   Alessandra; Hick, P. Paul L.; Eftekhari, Tarraneh; Yu, Hsiu-Shan;
   Odstrcil, Dusan; Tokumaru, Munetoshi
2016shin.confE..34B    Altcode:
  Observations of Faraday rotation (FR) can be used as a remote-sensing
  method of determining magnetic fields which has been well demonstrated
  through the corona, ionosphere, and interstellar medium. FR values
  are obtained via observations of polarised radio sources with
  well-documented characteristics (astronomical radio sources observed
  are typically Pulsars). Measurements of the inner corona of the Sun
  in FR have been shown from both spacecraft beacons and some natural
  radio sources but at relatively-high radio frequencies. Here we show
  some initial results of true heliospheric FR using the Low Frequency
  Array (LOFAR) below 200 MHz to investigate the passage of a coronal
  mass ejection (CME) across the line of sight. LOFAR is arguably
  the most-advanced interferometer radio telescope at present with
  wide-ranging radio-astronomy capabilities from imaging to beam forming
  multiple beams on the sky. We demonstrate preliminary heliospheric FR
  results through the analysis of observations of pulsar J1022+1001, which
  commenced on 13 August 2014 at 13:00UT and spanned over 150 minutes
  in duration. We also show initial comparisons to the FR results via
  modelling techniques and additional context information to understand
  the structure of the inner heliosphere being detected. This observation
  could pave the way to a set of observations and modelling techniques
  that might be implemented for space-weather purposes eventually leading
  to a near-global method for determining the magnetic field throughout
  the inner heliosphere. The most-intense space weather at Earth is
  due to geomagnetic storms. They are driven by the speed, density, and
  magnetic-field of the incoming plasma. The most-important determining
  factor of the intensity of geomagnetic storms is that of the North-South
  component of magnetic field (Bz in Geocentric Solar Magnetic - GSM
  - coordinates). Currently, there is no reliable prediction of this
  magnetic-field component until the incoming plasma from the Sun has
  reached in-situ monitors around the L1 point and this provides only
  15-60 minutes advanced warning.

---------------------------------------------------------
Title: Data driven modeling of the heliosphere using MS-FLUKSS
Authors: Kim, Tae K.; Pogorelov, Nikolai V.; Arge, C. Nick; Caplan,
   Ronald M.; Elliott, Heather A.; Jackson, Bernard V.; Linker, Jon A.;
   Lionello, Roberto; Manoharan, P. K.; McComas, David J.; Yu, Hsiu-Shan;
   Zank, Gary P.
2016shin.confE.188K    Altcode:
  The solar wind is a turbulent medium with physical properties
  fluctuating on multiple scales. We model the three-dimensional,
  time-dependent solar wind plasma flow using our own complications when
  multiple fluid species are introduced. We suggest space application
  of an alternative multi-fluid moment approach, treating each species
  on equal footing using exact evolution equations for moments of their
  distribution function, and electromagnetic fields through full Maxwell
  equations. Non-ideal effects like Hall effect, inertia, and even
  tensorial pressures, are self-consistently embedded without the need
  to explicitly solve a complicated Ohm's law. We have benchmarked this
  approach in classical test problems like the Orszag-Tang vortex and
  GEM reconnection problems, while also making significant progress in
  application to, for example, the magnetosphere of Ganymede. Coupling
  to state-of-art global simulation codes like OpenGGCM is also
  underway. This preparatory validation work, though treating only two
  species currently, shows the simplicity and power of the multi-fluid
  moment approach in space applications.

---------------------------------------------------------
Title: Exploration of SOLIS and GONG Data Sets Using the UCSD ISEE
    IPS Time-Dependent Tomography and the CSSS Magnetic Field Model
Authors: Jackson, Bernard Vernon; Yu, Hsiu-Shan; Buffington, Andrew;
   Hick, P. Paul; Nishimura, Nobuhiko; Nozaki, Nishiki; Tokumaru,
   Munetoshi; Fujiki, Ken'ichi; Hayashi, Keiji
2016shin.confE..54J    Altcode:
  We investigate daily Synoptic Optical Long-term Investigations of the
  Sun (SOLIS), and Global Oscillation Network Group (GONG) magnetograms
  extrapolated into the corona using Current-Sheet Source Surface
  (CSSS) modeling. The usual 'open-field' way to do this (Zhao &amp;
  Hoeksema, 1995 JGR 100, 19), and a closed-field extrapolation of the
  interplanetary magnetic field developed using this same modeling
  technique by the University of California, San Diego (UCSD), are
  compared with one another and with ACE component RTN fields measured
  near Earth. UCSD tomography (which assumes conservation of mass and
  mass flux), together with interplanetary scintillation (IPS) data from
  the Institute for Space-Earth Environmental Research (ISEE), Japan,
  provide global velocities and an accurate timing outward from the
  corona to Earth. Although the open-field technique generally gives a
  better result for radial and tangential fields, we find that a portion
  of the closed extrapolated fields measured in situ near Earth comes
  from the direct outward mapping of closed fields at the low solar
  corona. All three closed-field components are present at 1 AU, and
  are compared with the appropriate magnetometer values. A significant
  positive correlation exists between these closed loop components and
  the in-situ measurements over the last ten years. We determine that a
  small fraction of the static low-coronal component flux, that includes
  the Bn (north-south) component, regularly escapes from closed-field
  regions. The variation of this flux fraction is about a factor of
  three from 1.5% to 4% during this period, relative to the magnitude
  of the field components measured in situ near Earth: the implication
  is that a relatively more efficient process for closed flux escape
  occurs near solar maximum.

---------------------------------------------------------
Title: Measurements and an empirical model of the Zodiacal brightness
    as observed by the Solar Mass Ejection Imager (SMEI)
Authors: Buffington, Andrew; Bisi, Mario M.; Clover, John M.; Hick,
   P. Paul; Jackson, Bernard V.; Kuchar, Thomas A.; Price, Stephan D.
2016Icar..272...88B    Altcode:
  The Solar Mass Ejection Imager (SMEI) provided near-full-sky broadband
  visible-light photometric maps for 8.5 years from 2003 to 2011. At
  a cadence of typically 14 maps per day, these each have an angular
  resolution of about 0.5º 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. This sky coverage enables
  the formation of an empirical zodiacal-light model for observations at
  1 AU which summarizes the SMEI data. When this is subtracted, analysis
  of the ensemble of residual sky maps sets upper limits of typically
  1% for potential secular change of the zodiacal light for each of
  nine chosen ecliptic sky locations. An overall long-term photometric
  stability of 0.25% is certified by analysis of three stable sidereal
  objects. Averaging the nine ecliptic results together yields a 1-σ
  upper limit of 0.3% for zodiacal light change over this 8.5 year period.

---------------------------------------------------------
Title: A 17 June 2011 polar jet and its presence in the background
    solar wind
Authors: Yu, H. -S.; Jackson, B. V.; Yang, Y. -H.; Chen, N. -H.;
   Buffington, A.; Hick, P. P.
2016JGRA..121.4985Y    Altcode:
  High-speed jet responses in the polar solar wind are enigmatic. Here we
  measure a jet response that emanates from the southern polar coronal
  hole on 17 June 2011 at the extreme speed of over 1200 km/s. This
  response was recorded from the Sun-Earth line in Solar Dynamics
  Observatory/Atmospheric Imaging Assembly (SDO/AIA) and Large Angle
  and Spectrometric Coronagraph/C2 and both Solar TErrestrial RElations
  Observatory Extreme Ultraviolet Imager and COR2 coronagraphs when the
  three spacecraft were situated ~90° from one another. These certify
  the coronal 3-D location of the response that is associated with an
  existing solar plume structure and show its high speed to distances of
  over 14 R<SUB>S</SUB>. This jetting is associated with magnetic flux
  changes in the polar region as measured by the SDO/Helioseismic and
  Magnetic Imager instrumentation over a period of several hours. The
  fastest coronal response observed can be tracked to a time near the
  period of greatest flux changes and to the onset of the brightest
  flaring in AIA. This high-speed response can be tracked directly as a
  small patch of outward moving brightness in coronal images as in Yu et
  al. (2014) where three slower events were followed from the perspective
  of Earth. This accumulated jet response has the largest mass and energy
  we have yet seen in 3-D reconstructions from Solar Mass Ejection Imager
  observations, and its outward motion is certified for the first time
  using interplanetary scintillation observations. This jet response is
  surrounded by similar high-speed patches, but these are smoothed out
  in Ulysses polar measurements, we speculate about how these dynamic
  activities relate to solar wind acceleration.

---------------------------------------------------------
Title: Nova Light Curves From The Solar Mass Ejection Imager (SMEI)
    - II. The extended catalog
Authors: Hounsell, R.; Darnley, M. J.; Bode, M. F.; Harman, D. J.;
   Surina, F.; Starrfield, S.; Holdsworth, D. L.; Bewsher, D.; Hick,
   P. P.; Jackson, B. V.; Buffington, A.; Clover, J. M.; Shafter, A. W.
2016ApJ...820..104H    Altcode: 2015arXiv151203321H
  We present the results from observing nine Galactic novae in eruption
  with the Solar Mass Ejection Imager (SMEI) between 2004 and 2009. While
  many of these novae reached peak magnitudes that were either at
  or approaching the detection limits of SMEI, we were still able
  to produce light curves that in many cases contained more data at
  and around the initial rise, peak, and decline than those found in
  other variable star catalogs. For each nova, we obtained a peak time,
  maximum magnitude, and for several an estimate of the decline time
  ({t}<SUB>{{2</SUB>}}). Interestingly, although of lower quality than
  those found in Hounsell et al., two of the light curves may indicate
  the presence of a pre-maximum halt. In addition, the high cadence
  of the SMEI instrument has allowed the detection of low-amplitude
  variations in at least one of the nova light curves.

---------------------------------------------------------
Title: 3D Analysis of Remote-Sensed Heliospheric Data for Space
    Weather Forecasting
Authors: Yu, H. S.; Jackson, B. V.; Hick, P. P.; Buffington, A.;
   Bisi, M. M.; Odstrcil, D.; Hong, S.; Kim, J.; Yi, J.; Tokumaru, M.;
   Gonzalez-Esparza, A.
2015AGUFMSH21B2396Y    Altcode:
  The University of California, San Diego (UCSD) time-dependent iterative
  kinematic reconstruction technique has been used and expanded upon
  for over two decades. It currently provides some of the most accurate
  predictions and three-dimensional (3D) analyses of heliospheric
  solar-wind parameters now available using interplanetary scintillation
  (IPS) data. The parameters provided include reconstructions of velocity,
  density, and magnetic fields. Precise time-dependent results are
  obtained at any solar distance in the inner heliosphere using current
  Solar-Terrestrial Environment Laboratory (STELab), Nagoya University,
  Japan IPS data sets, but the reconstruction technique can also
  incorporate data from other IPS systems from around the world. With
  access using world IPS data systems, not only can predictions using
  the reconstruction technique be made without observation dead times
  due to poor longitude coverage or system outages, but the program can
  itself be used to standardize observations of IPS. Additionally, these
  analyses are now being exploited as inner-boundary values to drive
  an ENLIL 3D-MHD heliospheric model in real time. A major potential of
  this is that it will use the more realistic physics of 3D-MHD modeling
  to provide an automatic forecast of CMEs and corotating structures up
  to several days in advance of the event/features arriving at Earth,
  with or without involving coronagraph imagery or the necessity of
  magnetic fields being used to provide the background solar wind speeds.

---------------------------------------------------------
Title: Observations of Heliospheric Faraday Rotation (FR) and
    Interplanetary Scintillation (IPS) with the LOw Frequency ARray
(LOFAR): Steps Towards Improving Space-Weather Forecasting
    Capabilities
Authors: Bisi, M. M.; Fallows, R. A.; Sobey, C.; Eftekhari, T.;
   Jensen, E. A.; Jackson, B. V.; Yu, H. S.; Hick, P. P.; Odstrcil, D.;
   Tokumaru, M.
2015AGUFMSH21B2399B    Altcode:
  The phenomenon of space weather - analogous to terrestrial weather
  which describes the changing pressure, temperature, wind, and humidity
  conditions on Earth - is essentially a description of the changes in
  velocity, density, magnetic field, high-energy particles, and radiation
  in the near-Earth space environment including the effects of such
  changes on the Earth's magnetosphere, radiation belts, ionosphere,
  and thermosphere. Space weather can be considered to have two main
  strands: (i) scientific research, and (ii) applications. The former
  is self-explanatory, but the latter covers operational aspects which
  includes its forecasting. Understanding and forecasting space weather
  in the near-Earth environment is vitally important to protecting our
  modern-day reliance (militarily and commercially) on satellites,
  global-communication and navigation networks, high-altitude
  air travel (radiation concerns particularly on polar routes),
  long-distance power/oil/gas lines and piping, and for any future human
  exploration of space to list but a few. Two ground-based radio-observing
  remote-sensing techniques that can aid our understanding and forecasting
  of heliospheric space weather are those of interplanetary scintillation
  (IPS) and heliospheric Faraday rotation (FR). The LOw Frequency ARray
  (LOFAR) is a next-generation 'software' radio telescope centered in
  The Netherlands with international stations spread across central and
  northwest Europe. For several years, scientific observations of IPS
  on LOFAR have been undertaken on a campaign basis and the experiment
  is now well developed. More recently, LOFAR has been used to attempt
  scientific heliospheric FR observations aimed at remotely sensing
  the magnetic field of the plasma traversing the inner heliosphere. We
  present our latest progress using these two radio heliospheric-imaging
  remote-sensing techniques including the use of three-dimensional (3-D)
  modeling and reconstruction techniques using other, additional data
  as input (such as IPS data from the Solar Terrestrial Environment
  Laboratory - STELab) to support and better-interpret the LOFAR results.

---------------------------------------------------------
Title: Measurements and an Empirical Model of the Zodiacal Brightness
    as Observed by the Solar Mass Ejection Imager (SMEI)
Authors: Buffington, A.; Bisi, M. M.; Clover, J. M.; Hick, P. P.;
   Jackson, B. V.; Kuchar, T. A.; Price, S. D.
2015AGUFMSH53B2501B    Altcode:
  The Solar Mass Ejection Imager (SMEI) has provided near-full-sky
  broadband visible-light photometric maps for 8.5 years from 2003 to
  2011. These have an angular resolution of about 0.5º and differential
  photometric stability of about 1% per map 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. This sky coverage enables the formation of an empirical
  zodiacal-light model for observations at 1 AU which summarizes the
  SMEI data. When this is subtracted, analysis of the ensemble of
  residual sky maps sets upper limits of typically 1% for potential
  secular change of the zodiacal light for each of nine chosen ecliptic
  sky locations. An overall long-term photometric stability of 0.25%
  is certified by analysis of three stable sidereal objects. Averaging
  the nine ecliptic results together yields a 1-σ upper limit of 0.3%
  for zodiacal light change over this 8.5 year period.

---------------------------------------------------------
Title: Using In Situ and Remote Sensing Data to Model the Plasma
    Flow throughout the Heliosphere
Authors: Kim, T. K.; Pogorelov, N. V.; Arge, C. N.; Jackson, B. V.;
   Kryukov, I.; Manoharan, P. K.; Tropf, D.; Yu, H. S.; Zank, G. P.
2015AGUFMSH31C2441K    Altcode:
  The solar wind is a turbulent medium with physical properties
  fluctuating on multiple scales. We model three-dimensional solar wind
  plasma flow using our own software, Multi-Scale Fluid-Kinetic Simulation
  Suite, which, in addition to the thermal solar wind plasma, takes
  into account charge exchange of solar wind protons with interstellar
  neutral atoms and treats nonthermal ions (pickup ions, PUIs) born during
  this process as a separate fluid. Additionally, our model includes a
  description of turbulence generated by PUIs. For this investigation,
  we run our model using plasma and turbulence parameters from OMNI data
  as time-dependent boundary conditions at 1 AU for the Reynolds-averaged
  MHD equations and investigate the evolution of plasma and turbulent
  fluctuations along the trajectory of the New Horizons spacecraft,
  which recently passed by Pluto nearly ten years after launch. We
  also present solar wind simulations starting at 0.1 AU outwards using
  interplanetary scintillation data as boundary conditions. Simulations
  are compared with OMNI and STEREO data. The purpose of this study is
  to create a time-dependent solar wind model capable of reproducing the
  plasma flow, magnetic field, and turbulence along the trajectories of
  Solar Probe Plus and Solar Orbiter.

---------------------------------------------------------
Title: How Reliable Is the Solar Wind Prediction from the Models
    Installed at the CCMC?
Authors: Jian, L.; MacNeice, P. J.; Taktakishvili, A.; Odstrcil, D.;
   Jackson, B. V.; Yu, H. S.; Riley, P.; Sokolov, I.
2015AGUFMSH14A..08J    Altcode:
  The prediction of solar wind background is a necessary part of space
  weather forecasting. Multiple coronal and heliospheric models have
  been installed and/or recently upgraded at the Community Coordinated
  Modeling Center (CCMC) to produce the solar wind. They include the
  Wang-Sheely-Arge (WSA)-Enlil model, MHD-Around-a-Sphere (MAS)-Enlil
  model, Space Weather Modeling Framework (SWMF), and heliospheric
  tomography using the interplanetary scintillation (IPS) data. By
  comparing the modeling results with the OMNI and Ulysses data over seven
  Carrington rotations in 2007, we have conducted a third-party validation
  of these models for the near-Earth solar wind and the solar wind at
  mid-to-high latitudes, respectively. We have developed comprehensive
  performance metrics for solar wind simulation, which can be adapted
  to future model validation. The performance metrics include visual
  comparison, assessment of the time series and statistics of solar wind
  parameters, evaluation focused on the magnetic field sector boundaries
  (SBs) and slow-to-fast stream interaction regions (SIRs). General
  strengths and weaknesses for each model are diagnosed to provide an
  unbiased reference to model developers and users. For this period, the
  2014 version of MAS-Enlil model works best for SBs; the heliospheric
  tomography works best for SIRs; while the 2012 version of SWMF model
  works best for fast wind at mid-to-high latitudes. This work will help
  these models get ready for the transition from research to operation.

---------------------------------------------------------
Title: The first super geomagnetic storm of solar cycle 24: "The
    St. Patrick day (17 March 2015)" event
Authors: Wu, C. C.; Liou, K.; Socker, D. G.; Howard, R.; Jackson,
   B. V.; Yu, H. S.; Hutting, L.; Plunkett, S. P.
2015AGUFMSH51A2433W    Altcode:
  The first super geomagnetic storm of solar cycle 24 occurred on the
  "St. Patrick's day" (17 March 2015). Notably, it was a two-step
  storm. The source of the storm can be traced back to the solar event
  on March 15, 2015. At ~2:10 UT on that day, SOHO/LASCO C3 recorded
  a partial halo corona mass ejection (CME) which was associated with
  a C9.1/1F flare (S22W25) and a series of type II/IV radio bursts. The
  propagation speed of this CME is estimated to be ~668 km/s during 02:10
  - 06:20 UT (Figure 1). An interplanetary (IP) shock, likely driven by
  the CME, arrived at the Wind spacecraft at 03:59 UT on 17 March (Figure
  2). The arrival of the IP shock at the Earth may have caused a sudden
  storm commencement (SSC) at 04:45 UT on March 17. The storm intensified
  (Dst dropped to -80 nT at ~10:00 UT) during the crossing of the CME
  sheath. Later, the storm recovered slightly (Dst ~ -50 nT) after the
  IMF turned northward. At 11:01 UT, IMF started turning southward again
  due to the large magnetic cloud (MC) field itself and caused the second
  storm intensification, reaching Dst = - 228 nT on March 18. We conclude
  that the St. Patrick day event is a two-step storm. The first step
  is associated with the sheath, whereas the second step is associated
  with the MC. Here, we employ a numerical simulation using the global,
  three-dimensional (3D), time-dependent, magnetohydrodynamic (MHD)
  model (H3DMHD, Wu et al. 2007) to study the CME propagation from the
  Sun to the Earth. The H3DMHD model has been modified so that it can be
  driven by (solar wind) data at the inner boundary of the computational
  domain. In this study, we use time varying, 3D solar wind velocity and
  density reconstructed from STELab, Japan interplanetary scintillation
  (IPS) data by the University of California, San Diego, and magnetic
  field at the IPS inner boundary provided by CSSS model closed-loop
  propagation (Jackson et a., 2015). The simulation result matches well
  with the in situ solar wind plasma and field data at Wind, in terms of
  the peak values of the IP shock and its arrival time (Figure 3). The
  simulation not only helps us to identify the driver of the IP shock,
  but also demonstrates that the modified H3DMHD model is capable of
  realistic simulations of large solar event. In this presentation, we
  will discuss the CME/storm event with detailed data from observations
  (Wind and SOHO) and our numerical simulation.

---------------------------------------------------------
Title: Determination of the North-South Heliospheric Magnetic-Field
    Component from Inner-Corona Closed-Loop Propagation
Authors: Jackson, B. V.; Yu, H. S.; Hick, P. P.; Buffington, A.;
   Bisi, M. M.; Tokumaru, M.; Kim, J.; Hong, S.; Lee, B.; Yi, J.; Yun, J.
2015AGUFMSH43C..03J    Altcode:
  We find that a portion of the north-south interplanetary magnetic field
  measured in situ near Earth is present from a direct outward mapping
  of closed fields from the low solar corona. Using the Current-Sheet
  Source Surface (CSSS) model (Zhao &amp; Hoeksema, 1995 JGR 100, 19),
  these lower coronal fields are extrapolated upward from near the solar
  surface. Global velocities inferred from a combination of observations
  of interplanetary scintillation (IPS) matched to in-situ velocities
  and densities measured by spacecraft instrumentation provide an
  accurate outward timing to 1 AU from a model assuming conservation
  of mass and mass flux. The north-south field component at 1 AU is
  compared with the appropriate ACE magnetometer in-situ Normal (RTN)
  or Bn field coordinate (Jackson et al., 2015, ApJL, 803:L1). From a
  significant positive correlation between this method of determining
  the Bn field compared with in-situ measurements over a three-year
  period during the last solar minimum, we find that a small fraction
  of the low-coronal Bn component flux (~1%) regularly escapes from
  closed-field regions. Since the Bn field provides the major portion
  of the Geocentric Solar Magnetospheric (GSM) Bz field component that
  couples most closely to the Earth's geomagnetic field, the prospects
  for its determination using this technique for space weather use are
  being actively developed by our many colleague groups.

---------------------------------------------------------
Title: Requirements for an Operational Coronagraph
Authors: Howard, R.; Vourlidas, A.; Harrison, R. A.; Bisi, M. M.;
   Plunkett, S. P.; Socker, D. G.; Eyles, C. J.; Webb, D. F.; DeForest,
   C. E.; Davies, J. A.; Howard, T. A.; de Koning, C. A.; Gopalswamy,
   N.; Davila, J. M.; Tappin, J.; Jackson, B. V.
2015AGUFMSH14A..02H    Altcode:
  Coronal mass ejections (CMEs) have been shown to be the major driver
  of the non-recurrent space weather events and geomagnetic storms. The
  utility of continuously monitoring such events has been very effectively
  demonstrated by the LASCO experiment on the SOHO mission. However SOHO
  is aging, having been launched 20 years ago on Dec 2, 1995. The STEREO
  mission, in which two spacecraft in orbits about the sun are drifting
  away from earth, has shown the utility of multiple viewpoints off the
  sun-earth line. Up to now the monitoring of CMES has been performed
  by scientific instruments such as LASCO and SECCHI with capabilities
  beyond those required to record the parameters that are needed to
  forecast the impact at earth. However, there is great interest within
  the US NOAA and the UK Met Office to launch operational coronagraphs
  to L1 and L5. An ad-hoc group was formed to define the requirements
  of the L5 coronagraph. In this paper we present some requirements that
  must be met by operational coronagraphs. The Office of Naval Research
  is gratefully acknowledged.

---------------------------------------------------------
Title: Comparison of Solar Wind Speeds Using Wavelet Transform and
    Fourier Analysis in IPS Data
Authors: Aguilar-Rodriguez, E.; Mejia-Ambriz, J. C.; Jackson, B. V.;
   Buffington, A.; Romero-Hernandez, E.; Gonzalez-Esparza, J. A.;
   Rodriguez-Martinez, M.; Hick, P.; Tokumaru, M.; Manoharan, P. K.
2015SoPh..290.2507A    Altcode: 2015SoPh..tmp..123A
  The power spectra of intensity fluctuations in interplanetary
  scintillation (IPS) observations can be used to estimate solar-wind
  speeds in the inner heliosphere. We obtain and then compare IPS
  spectra from both wavelet and Fourier analyses for 12 time series
  of the radio source 3C48; these observations were carried out at
  Japan's Solar-Terrestrial Environment Laboratory (STEL) facility, at
  327 MHz. We show that wavelet and Fourier analyses yield very similar
  power spectra. Thus, when fitting a model to spectra to determine
  solar-wind speeds, both yield comparable results. Although spectra
  from wavelet and Fourier closely match each other for solar-wind speed
  purposes, those from the wavelet analysis are slightly cleaner, which
  is reflected in an apparent level of intensity fluctuations that is
  enhanced, being ≈ 13 % higher. This is potentially useful for records
  that show a low signal-to-noise ratio.

---------------------------------------------------------
Title: Remote-Sensing of Solar Wind Speeds from IPS Observations at
    140 and 327 MHz Using MEXART and STEL
Authors: Mejia-Ambriz, J. C.; Jackson, B. V.; Gonzalez-Esparza, J. A.;
   Buffington, A.; Tokumaru, M.; Aguilar-Rodriguez, E.
2015SoPh..290.2539M    Altcode: 2015SoPh..tmp...53M
  Interplanetary scintillation (IPS) is used to probe solar wind speeds
  in the inner heliosphere by applying either of two generalized
  data-analysis techniques: model fitting to power spectra (MFPS)
  from a single station, or cross-correlation functions (CCF) produced
  by cross-correlating two simultaneous IPS time series from separate
  stations. The MEXican Array Radio Telescope (MEXART), observing at 140
  MHz, is starting to use an MFPS technique. Here we report the first
  successful solar wind speed determinations with IPS observations by
  MEXART. Three stations of the Solar-Terrestrial Environment Laboratory
  (STEL), observing at 327 MHz, use a CCF, and an MFPS technique is also
  used at one of these sites. We here analyze data from MEXART and from
  one antenna of STEL to obtain solar wind speeds using an MFPS technique
  from a single station. The IPS observations were carried out with radio
  source 3C48 during Solar Cycle 24. The MFPS method we describe here is
  tested by comparing its obtained speeds with those from the STEL CCF
  technique. We find that the speeds from the two techniques generally
  agree within the estimated errors.

---------------------------------------------------------
Title: Preface: Radio Heliophysics: Science and Forecasting
Authors: Bisi, Mario M.; Americo Gonzalez-Esparza, J.; Jackson,
   Bernard V.; Tokumaru, Munetoshi; Leibacher, John
2015SoPh..290.2393B    Altcode: 2015SoPh..tmp..143B
  No abstract at ADS

---------------------------------------------------------
Title: 3D Reconstruction of Interplanetary Scintillation (IPS)
Remote-Sensing Data: Global Solar Wind Boundaries for Driving
    3D-MHD Models
Authors: Yu, H. -S.; Jackson, B. V.; Hick, P. P.; Buffington, A.;
   Odstrcil, D.; Wu, C. -C.; Davies, J. A.; Bisi, M. M.; Tokumaru, M.
2015SoPh..290.2519Y    Altcode: 2015SoPh..tmp...47Y
  The University of California, San Diego, time-dependent analyses of the
  heliosphere provide three-dimensional (3D) reconstructions of solar
  wind velocities and densities from observations of interplanetary
  scintillation (IPS). Using data from the Solar-Terrestrial
  Environment Laboratory, Japan, these reconstructions provide a
  real-time prediction of the global solar-wind density and velocity
  throughout the whole heliosphere with a temporal cadence of about one
  day (ips.ucsd.edu). Updates to this modeling effort continue: in the
  present article, near-Sun results extracted from the time-dependent
  3D reconstruction are used as inner boundary conditions to drive
  3D-MHD models (e.g. ENLIL and H3D-MHD). This allows us to explore the
  differences between the IPS kinematic-model data-fitting procedure and
  current 3D-MHD modeling techniques. The differences in these techniques
  provide interesting insights into the physical principles governing
  the expulsion of coronal mass ejections (CMEs). Here we detail for the
  first time several specific CMEs and an induced shock that occurred
  in September 2011 that demonstrate some of the issues resulting from
  these analyses.

---------------------------------------------------------
Title: A 3D-MHD Model Interface Using Interplanetary Scintillation
    (IPS) Observations
Authors: Jackson, Bernard V.; Yu, H. -S.; Hick, P. P.; Buffington,
   A.; Odstrcil, D.; Kim, T. K.; Pogorelov, N. V.; Wu, C. -C.; Tokumaru,
   M.; Kim, J.; Hong, S.
2015shin.confE..95J    Altcode:
  We at UCSD for over two decades have developed a remote-sensing
  iterative time-dependent three-dimensional (3D) tomographic
  reconstruction technique which provides volumetric maps of density,
  velocity, and magnetic field. These extend from an inner boundary out to
  nearly the whole inner heliosphere. This modeling requires a "traceback"
  to the boundary, from any element within the heliospheric volume, which
  specifies the element origin, time, and change from a 2D location on a
  set of Carrington maps. Moreover, this process has recently included
  a traceback from any input volume to yield an updated boundary in
  velocity, density, temperature, and magnetic field components, based
  on fitting to data from interplanetary scintillation (IPS) or other
  remotely-sensed heliospheric measurements. This traceback from an
  external volume is the most difficult step needed to implement a future
  UCSD iterative tomographic analysis from any given solar-wind model. Up
  to now, the iterative UCSD tomographic analysis (fitting STELab, Japan,
  IPS data) has used an internal solar wind model that conserves mass
  and mass flux, and as a first step allows an inner boundary to be
  extracted to drive heliospheric 3D-MHD (magnetohydrodynamic) forward
  models. Here, three examples are shown where this IPS inner boundary
  has been used in this way: 1) Analysis of the 9-10 September 2014 halo
  coronal mass ejections (CMEs) using the ENLIL 3D-MHD code at Earth and
  at the Rosetta spacecraft situated at 3.7 AU; 2) Analysis of the period
  during two halo CMEs on 24 September 2011 using the MS-FLUKSS UAH 3D-MHD
  heliospheric code; 3) Analysis of the 15 March 2015 halo CME and its
  associated three component magnetic fields with the NRL H3D-MHD code.

---------------------------------------------------------
Title: Use of ground based, remote sensing and in situ measurements
    as boundary conditions in MS-FLUKSS to simulate the interplanetary
    plasma flow
Authors: Kim, Tae Kwang; Pogorelov, N. V.; Arge, C. N.; Caplan, R.;
   Jackson, B. V.; Linker, J. A.; Lionello, R.; Yu, H. -S.; Zank, G. P.
2015shin.confE..48K    Altcode:
  The solar wind is a turbulent medium with fluctuating physical
  properties in both small and large scales where interactions between
  co-rotating features and/or transient structures such as CMEs play
  a significant role. The accuracy of numerical models largely depends
  on the quality of the boundary conditions that drive them. We explore
  various sources of time-varying boundary conditions used with the 3-D
  heliospheric MHD code developed at UAH. Supported by the SHINE program,
  we are currently in the process of iteratively fitting the MHD model
  to interplanetary scintillation observations. We also use OMNI data
  to propagate the solar wind from 1 AU to the outer heliosphere while
  taking turbulence and pickup ions into account which become increasingly
  important beyond 5 AU. The preliminary results along the trajectories
  of Pluto and the New Horizons spacecraft are shown here. Additionally,
  we have used the Wang-Sheeley-Arge (WSA) solutions from the Air Force
  Data Assimilative Photospheric flux Transport (ADAPT) maps directly
  as inner boundary conditions to simulate the background solar wind
  outflow from 0.1 AU. Furthermore, we show comparisons between our
  model and Magnetohydrodynamics Around a Sphere (MAS) solutions at 1 AU
  for which we have used the ADAPT-DCHB(distance from the coronal hole
  boundary)-MAS solutions at 40 solar radii as inner boundary conditions.

---------------------------------------------------------
Title: How Reliable Is the Prediction of Solar Wind Background?
Authors: Jian, Lan K.; MacNeice, Peter; Taktakishvili, Aleksandre;
   Odstrcil, Dusan; Jackson, Bernard; Yu, Hsiu-Shan; Riley, Pete;
   Sokolov, Igor
2015TESS....120001J    Altcode:
  The prediction of solar wind background is a necessary part of space
  weather forecasting. Multiple coronal and heliospheric models have
  been installed at the Community Coordinated Modeling Center (CCMC)
  to produce the solar wind, including the Wang-Sheely-Arge (WSA)-Enlil
  model, MHD-Around-a-Sphere (MAS)-Enlil model, Space Weather Modeling
  Framework (SWMF), and heliospheric tomography using interplanetary
  scintillation (IPS) data. By comparing the modeling results with the
  OMNI data over 7 Carrington rotations in 2007, we have conducted
  a third-party validation of these models for the near-Earth solar
  wind. This work will help the models get ready for the transition from
  research to operation. Besides visual comparison, we have quantitatively
  assessed the models’ capabilities in reproducing the time series
  and statistics of solar wind parameters. Using improved algorithms, we
  have identified magnetic field sector boundaries (SBs) and slow-to-fast
  stream interaction regions (SIRs) as focused structures. The success
  rate of capturing them and the time offset vary largely with models. For
  this period, the 2014 version of MAS-Enlil model works best for SBs,
  and the heliospheric tomography works best for SIRs. General strengths
  and weaknesses for each model are identified to provide an unbiased
  reference to model developers and users.

---------------------------------------------------------
Title: A Determination of the North-South Heliospheric Magnetic
    Field Component from Inner Corona Closed-loop Propagation
Authors: Jackson, B. V.; Hick, P. P.; Buffington, A.; Yu, H. -S.;
   Bisi, M. M.; Tokumaru, M.; Zhao, X.
2015ApJ...803L...1J    Altcode:
  A component of the magnetic field measured in situ near the Earth in
  the solar wind is present from north-south fields from the low solar
  corona. Using the Current-sheet Source Surface model, these fields
  can be extrapolated upward from near the solar surface to 1 AU. Global
  velocities inferred from a combination of interplanetary scintillation
  observations matched to in situ velocities and densities provide the
  extrapolation to 1 AU assuming mass and mass flux conservation. The
  north-south field component is compared with the same ACE in situ
  magnetic field component—the Normal (Radial Tangential Normal)
  Bn coordinate—for three years throughout the solar minimum of
  the current solar cycle. We find a significant positive correlation
  throughout this period between this method of determining the Bn field
  compared with in situ measurements. Given this result from a study
  during the latest solar minimum, this indicates that a small fraction
  of the low-coronal Bn component flux regularly escapes from closed
  field regions. The prospects for Space Weather, where the knowledge
  of a Bz field at Earth is important for its geomagnetic field effects,
  is also now enhanced. This is because the Bn field provides the major
  portion of the Geocentric Solar Magnetospheric Bz field coordinate
  that couples most closely to the Earth’s geomagnetic field.

---------------------------------------------------------
Title: Heliospheric Tomography from IPS Data at 140 MHz
Authors: Mejia-Ambriz, J. C.; Jackson, B. V.; Gonzalez-Esparza, A.;
   Buffington, A.
2014AGUFMSH33A4117M    Altcode:
  Interplanetary scintillation (IPS) from radio telescopes provides
  data to study density and velocity evolution of the solar wind and
  heliospheric disturbances. A tomography program developed at the
  University of California, San Diego, makes 3D reconstructions and
  forecasts of the inner heliosphere dynamics from IPS results. For the
  first time we incorporate 140 MHz IPS results from the MEXican Array
  Radio Telescope (MEXART) into the tomography program. We show that
  MEXART data complement observations from other radio-systems located
  at different longitudes, thus providing more complete heliospheric
  coverage.

---------------------------------------------------------
Title: A Challenging Solar Eruptive Event of 18 November 2003 and
    the Causes of the 20 November Geomagnetic Superstorm. IV. Unusual
    Magnetic Cloud and Overall Scenario
Authors: Grechnev, V. V.; Uralov, A. M.; Chertok, I. M.; Belov, A. V.;
   Filippov, B. P.; Slemzin, V. A.; Jackson, B. V.
2014SoPh..289.4653G    Altcode: 2014arXiv1409.0283G; 2014SoPh..tmp..125G
  The geomagnetic superstorm of 20 November 2003 with Dst=−422 nT,
  one of the most intense in history, is not well understood. The
  superstorm was caused by a moderate solar eruptive event on 18
  November, comprehensively studied in our preceding Papers I - III. The
  analysis has shown a number of unusual and extremely complex features,
  which presumably led to the formation of an isolated right-handed
  magnetic-field configuration. Here we analyze the interplanetary
  disturbance responsible for the 20 November superstorm, compare some
  of its properties with the extreme 28 - 29 October event, and reveal a
  compact size of the magnetic cloud (MC) and its disconnection from the
  Sun. Most likely, the MC had a spheromak configuration and expanded in
  a narrow angle of ≤ 14<SUP>∘</SUP>. A very strong magnetic field
  in the MC up to 56 nT was due to the unusually weak expansion of the
  disconnected spheromak in an enhanced-density environment constituted
  by the tails of the preceding ICMEs. Additional circumstances favoring
  the superstorm were i) the exact impact of the spheromak on the Earth's
  magnetosphere and ii) the almost exact southward orientation of the
  magnetic field, corresponding to the original orientation in its
  probable source region near the solar disk center.

---------------------------------------------------------
Title: Using IPS Magnetic Modeling to Determine Bz
Authors: Jackson, B. V.; Yu, H. S.; Hick, P. P.; Buffington, A.;
   Mejia-Ambriz, J. C.; Bisi, M. M.; Tokumaru, M.
2014AGUFMSH21C4144J    Altcode:
  Interplanetary scintillation (IPS) observations enable remote
  determinations of velocity and density in the inner heliosphere
  while also providing forecasts of these quantities. Using the global
  velocities inferred from IPS, and through convection upward of magnetic
  fields perpendicular to a source surface produced by the Current-Sheet
  Source Surface (CSSS) modified potential model (Zhao and Hoeksema,
  J. Geophys. Res., 100, 19, 1995), global long-duration radial and
  tangential heliospheric field components can also be determined. In
  order to better include short-term transient effects and derive a
  value for the field normal to these components (Bn) during periods
  where CMEs, are present, we have tested an extension to our current 3D
  vector-field analysis. This extension adds closed fields from below the
  source surface to the CSSS model values, and when traced outward from
  the sub-Earth point, three magnetic field components are present. These
  are compared to in-situ magnetic fields measured near Earth for several
  periods throughout the current solar cycle from the minimum between
  Solar Cycle 23 and 24 up until the present. We find a significant
  positive correlation when using this extension to current analyses
  including that of the Bn field for the test cases analyzed thus far.

---------------------------------------------------------
Title: On the Dynamic Character of the Polar Solar Wind
Authors: Yu, H. S.; Jackson, B. V.; Hick, P. P.; Buffington, A.
2014AGUFMSH13C4131Y    Altcode:
  SOHO LASCO C2 and STEREO SECCHI COR 2 coronagraph images, when
  analyzed using correlation tracking techniques, show a surprising
  result in polar coronal hole regions ordinarily thought of as "quiet"
  solar wind. Here what we observe is not the static well-ordered flow
  and gradual acceleration expected of quiescent regions. Rather, the
  coronagraph images show outflow in polar coronal holes as intermittent,
  highly-variable solar wind speed structures. We compare measurements
  of these structures in different simultaneously-measured coronagraph
  images, and with coronal brightness. The distribution of structure
  speeds shows a gradual decrease with speed in the overlap regions of
  the two coronagraphs. Measurements of the mean speed derived versus
  height shows the solar wind acceleration with position angle, and are
  compared with mass flux and other determinations of solar wind outflow
  over the large polar coronal hole regions. In this presentation we
  give the most recent work on this ongoing analysis.

---------------------------------------------------------
Title: Validation of Coronal and Heliospheric Models for Quasi-Steady
Solar Wind: WSA-Enlil, MAS-Enlil, SWMF, and IPS Tomography Models
Authors: Jian, L.; MacNeice, P. J.; Taktakishvili, A.; Evans, R. M.;
   Odstrcil, D.; Arge, C. N.; Jackson, B. V.; Yu, H. S.; Riley, P.;
   Sokolov, I.
2014AGUFMSH33A4118J    Altcode:
  Multiple coronal and heliospheric models have been recently upgraded
  at the Community Coordinated Modeling Center (CCMC), including the
  Wang-Sheely-Arge (WSA)-Enlil, MHD-around-a-sphere (MAS)-Enlil, space
  weather modeling framework (SWMF), and interplanetary scintillation
  (IPS) tomography models. We run these models for Carrington rotations
  2056 - 2062 (April - November 2007), in which the solar wind was in the
  late declining phase and Ulysses had a fast latitudinal scan at 1.4 -
  1.8 AU. We compare the modeling results with the in situ observations:
  OMNI data for L1, MESSENGER, Venus Express and Ulysses, all together
  covering 0.3 - 1.8 AU. We assess the capabilities of these models in
  capturing quasi-steady solar wind features including sector boundaries
  and the fast-slow stream interaction regions. For this particular
  period, we derive the strengths, weaknesses, and discrepancies from
  observations for each model, and discuss the effect of photospheric
  magnetograms from different observatories, such as GONG and SOLIS
  magnetograms from National Solar Observatory (NSO) and magnetograms
  from Mount Wilson Observatory (MWO).

---------------------------------------------------------
Title: Faraday Rotation (FR) and Interplanetary Scintillation (IPS)
    Case Studies Using the LOw Frequency ARray (LOFAR)
Authors: Bisi, M. M.; Fallows, R. A.; Sobey, C.; Eftekhari, T.;
   Jensen, E. A.; Jackson, B. V.; Yu, H. S.; Gershman, D. J.; Raines,
   J. M.; Odstrcil, D.
2014AGUFMSH21C4143B    Altcode:
  We present an update on the progress made using the LOw Frequency
  ARray (LOFAR) next-generation radio telescope for space-weather
  related activities - namely observations of interplanetary
  scintillation (IPS) and the first tests of observing heliospheric
  Faraday rotation (FR). The former has been used for half a century
  for heliospheric science and much progress has been made in recent
  years for using IPS in space weather science and forecasting. The
  latter, typically an astrophysical technique that uses pulsars and
  extragalactic radio sources to study the Galactic magnetic field, is
  now being investigated for heliospheric studies. The determination
  of heliospheric FR, combined with observations of IPS, can provide
  essential information on the Sun's extended magnetic-field structure
  out into the inner heliosphere, especially when also combined with
  other forms of remote-sensing/heliospheric imaging data, and in-situ
  measurements. Here, we will present recent observations of IPS using
  LOFAR, including preliminary highlights from the first LOFAR joint
  IPS and heliospheric FR science campaign and investigate pathways
  for determining Bzfrom, and an overview of the potential of, such
  observations. LOFAR is an interferometric phased-array radio telescope
  that can be used to observe between 10 MHz (depending on ionospheric
  conditions) and 240 MHz, and consists of many relatively-low-cost
  antennas. These antennas are organised into 'stations' located
  in an area of ~100km diameter in the Netherlands, with additional
  international stations spread across central and western Europe with
  several more in the planning stages.

---------------------------------------------------------
Title: An Ensemble Study of a January 2010 Coronal Mass Ejection
(CME): Connecting a Non-obvious Solar Source with Its ICME/Magnetic
    Cloud
Authors: Webb, D. F.; Bisi, M. M.; de Koning, C. A.; Farrugia, C. J.;
   Jackson, B. V.; Jian, L. K.; Lugaz, N.; Marubashi, K.; Möstl, C.;
   Romashets, E. P.; Wood, B. E.; Yu, H. -S.
2014SoPh..289.4173W    Altcode: 2014SoPh..tmp..114W
  A distinct magnetic cloud (MC) was observed in-situ at the Solar
  TErrestrial RElations Observatory (STEREO)-B on 20 - 21 January
  2010. About three days earlier, on 17 January, a bright flare and
  coronal mass ejection (CME) were clearly observed by STEREO-B,
  which suggests that this was the progenitor of the MC. However, the
  in-situ speed of the event, several earlier weaker events, heliospheric
  imaging, and a longitude mismatch with the STEREO-B spacecraft made this
  interpretation unlikely. We searched for other possible solar eruptions
  that could have caused the MC and found a faint filament eruption
  and the associated CME on 14 - 15 January as the likely solar source
  event. We were able to confirm this source by using coronal imaging
  from the Sun Earth Connection Coronal and Heliospheric Investigation
  (SECCHI)/EUVI and COR and Solar and Heliospheric Observatory
  (SOHO)/Large Angle and Spectrometric Coronograph (LASCO) telescopes
  and heliospheric imaging from the Solar Mass Ejection Imager (SMEI)
  and the STEREO/Heliospheric Imager instruments. We use several empirical
  models to understand the three-dimensional geometry and propagation of
  the CME, analyze the in-situ characteristics of the associated ICME, and
  investigate the characteristics of the MC by comparing four independent
  flux-rope model fits with the launch observations and magnetic-field
  orientations. The geometry and orientations of the CME from the
  heliospheric-density reconstructions and the in-situ modeling are
  remarkably consistent. Lastly, this event demonstrates that a careful
  analysis of all aspects of the development and evolution of a CME is
  necessary to correctly identify the solar counterpart of an ICME/MC.

---------------------------------------------------------
Title: MHD heliosphere with boundary conditions from a tomographic
    reconstruction using interplanetary scintillation data
Authors: Kim, T. K.; Pogorelov, N. V.; Borovikov, S. N.; Jackson,
   B. V.; Yu, H. -S.; Tokumaru, M.
2014JGRA..119.7981K    Altcode:
  Observations of interplanetary scintillation (IPS) provide a set
  of data that is used in estimating the solar wind parameters with
  reasonably good accuracy. Various tomography techniques have been
  developed to deconvolve the line-of-sight integration effects
  ingrained in observations of IPS to improve the accuracy of solar
  wind reconstructions. Among those, the time-dependent tomography
  developed at the University of California, San Diego (UCSD) is well
  known for its remarkable accuracy in reproducing the solar wind speed
  and density at Earth by iteratively fitting a kinematic solar wind model
  to observations of IPS and near-Earth spacecraft measurements. However,
  the kinematic model gradually breaks down as the distance from the Sun
  increases beyond the orbit of Earth. Therefore, it would be appropriate
  to use a more sophisticated model, such as a magnetohydrodynamics (MHD)
  model, to extend the kinematic solar wind reconstruction beyond the
  Earth's orbit and to the outer heliosphere. To test the suitability
  of this approach, we use boundary conditions provided by the UCSD
  time-dependent tomography to propagate the solar wind outward in a
  MHD model and compare the simulation results with in situ measurements
  and also with the corresponding kinematic solution. Interestingly, we
  find notable differences in proton radial velocity and number density
  at Earth and various locations in the inner heliosphere between the
  MHD results and both the in situ data and the kinematic solution. For
  example, at 1 AU, the MHD velocities are generally larger than the
  spacecraft data by up to 150 km s<SUP>-1</SUP>, and the amplitude of
  density fluctuations is also markedly larger in the MHD solution. We
  show that the MHD model can deliver more reasonable results at Earth
  with an ad hoc adjustment of the inner boundary values. However, we
  conclude that the MHD model using the inner boundary conditions derived
  from kinematic simulations has little chance to match IPS and in situ
  data as well as the kinematic model does unless it too is iteratively
  fit to the observational data and measurements.

---------------------------------------------------------
Title: The Dynamic Character of the Polar Solar Wind
Authors: Jackson, B. V.; Yu, H. -S.; Buffington, A.; Hick, P. P.
2014ApJ...793...54J    Altcode:
  The Solar and Heliospheric Observatory (SOHO) Large Angle and
  Spectrometric Coronagraph C2 and Solar Terrestrial Relations
  Observatory (STEREO) COR2A coronagraph images, when analyzed using
  correlation tracking techniques, show a surprising result in places
  ordinarily thought of as "quiet" solar wind above the poles in coronal
  hole regions. Instead of the static well-ordered flow and gradual
  acceleration normally expected, coronagraph images show outflow in polar
  coronal holes consisting of a mixture of intermittent slow and fast
  patches of material. We compare measurements of this highly variable
  solar wind from C2 and COR2A images and show that both coronagraphs
  measure essentially the same structures. Measurements of the mean
  velocity as a function of height of these structures are compared with
  mass flux determinations of the solar wind outflow in the large polar
  coronal hole regions and give similar results.

---------------------------------------------------------
Title: The UCSD Kinematic Global Solar Wind Boundary for use in
    real-time ENLIL 3D-MHD Modeling
Authors: Yu, Hsiu-Shan; Jackson, Bernard; Hick, Paul; Buffington,
   Andrew; Odstrcil, Dusan; Tokumaru, Munetoshi; Hong, Sunhak; Kim,
   Jaehun; Kim, Yungkyu
2014shin.confE..95Y    Altcode:
  The UCSD IPS time-dependent iterative kinematic modeling technique has
  been used and expanded-upon for over more than a decade to provide some
  of the most accurate forecasts of heliospheric solar-wind parameters
  now available. These parameters include global models of velocity,
  density, and through convection upward of magnetic fields from the
  solar surface, radial and tangential heliospheric fields. The precise
  time-dependent results can be extracted at any solar distance and are
  now being exploited as inner boundary values to drive the ENLIL and
  other 3D-MHD models. For ENLIL, this data-driven modeling effort is
  now available in real time. The advantage of this system is that it
  uses the superior physics of 3D-MHD modeling to provide an automatic
  forecast of CMEs and corotating structures several days in advance
  of the present at Earth without using coronagraph observations. Here,
  we explore the current differences between the IPS real-time kinematic
  analyses and those from the ENLIL 3D-MHD modeling using IPS-derived
  real-time boundaries.

---------------------------------------------------------
Title: The UCSD Kinematic Global Solar Wind Analysis Tests of
    Different Magnetogram Inputs using MAGIC
Authors: Jackson, Bernard V.; Hick, Paul; Buffington, Andrew; Yu,
   Hsiu-Shan; Mejia-Ambriz, Julio; MacNeice, Peter
2014shin.confE..96J    Altcode:
  The UCSD IPS time-dependent iterative kinematic modeling technique has
  been used and expanded-upon for over more than a decade to provide some
  of the most accurate forecasts of heliospheric solar-wind parameters
  now available. These parameters include global models of velocity,
  density, and through convection upward of magnetic fields from near the
  solar surface, radial and tangential heliospheric fields using the CSSS
  Potential Field Model (Zhao and Hoeksema, 1995, JGR, 100, 19). The RTN
  coordinate fields mapped to Earth and matched to in-situ measurements
  from L1 spacecraft can accurately reproduce daily or longer-term average
  field component values, but this accuracy depends on the magnetic field
  inputs from different ground and space-based sources. Here we use inputs
  provided by the newly-available MAGIC routine from the NASA-Goddard
  Community Coordinate Modeling Center (CCMC) to evaluate the differences
  present in the two RTN field coordinates. These are mapped to Earth
  and compared with near-Earth spacecraft magnetic field measurements for
  several different Carrington rotations from 2007 up to the present day.

---------------------------------------------------------
Title: Modeling the Global Heliosphere Using IPS-derived
    Time-dependent Boundary Conditions
Authors: Kim, T. K.; Pogorelov, N. V.; Borovikov, S. N.; Hayashi,
   K.; Jackson, B. V.; Tokumaru, M.; Yu, H.
2014ASPC..484...91K    Altcode:
  Interplanetary scintillation (IPS) observations are a well-known,
  powerful tool that has long been used in solar wind (SW) forecasting. In
  the last couple of decades, several tomography methods have been
  developed to reconstruct the time-varying three-dimensional SW
  structure from IPS observations with reasonably good accuracy out to
  several astronomical units beyond Earth's orbit. With some of these
  tomographic reconstructions at certain fixed heliocentric distances
  as time-dependent boundary conditions, we have simulated the plasma
  flow in the inner heliosphere magnetohydrodynamically (MHD) and in the
  outer heliosphere using an MHD-neutral model. Since the SW structure
  often changes significantly in time, the accuracy of the boundary
  conditions is particularly important in modeling the SW outflow in
  interplanetary space and the interaction between the SW and the local
  interstellar medium at the edge of the heliosphere. In this paper,
  we summarize our past and current efforts in modeling the global
  heliosphere using IPS-based time-varying boundary conditions and
  discuss how we may improve the accuracy of our SW reconstructions.

---------------------------------------------------------
Title: The Three-dimensional Analysis of Hinode Polar Jets using
    Images from LASCO C2, the Stereo COR2 Coronagraphs, and SMEI
Authors: Yu, H. -S.; Jackson, B. V.; Buffington, A.; Hick, P. P.;
   Shimojo, M.; Sako, N.
2014ApJ...784..166Y    Altcode:
  Images recorded by the X-ray Telescope on board 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 the 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 Solar Mass Ejection Imager (SMEI) 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.

---------------------------------------------------------
Title: The Solar Mass Ejection Imager and Its Heliospheric Imaging
    Legacy
Authors: 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. D.; Radick, R. R.; Simnett, G. M.; Tappin,
   S. J.; Waltham, N. R.; Webb, D. F.
2013SSRv..180....1H    Altcode: 2013SSRv..tmp...71H
  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.

---------------------------------------------------------
Title: Inclusion of Real-Time In-Situ Measurements into the UCSD
    Time-Dependent Tomography and Its Use as a Forecast Algorithm
Authors: Jackson, B. V.; Clover, J. M.; Hick, P. P.; Buffington, A.;
   Bisi, M. M.; Tokumaru, M.
2013SoPh..285..151J    Altcode: 2012SoPh..tmp..210J
  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.

---------------------------------------------------------
Title: Heliospheric Imaging of 3D Density Structures During the
    Multiple Coronal Mass Ejections of Late July to Early August 2010
Authors: Webb, D. F.; Möstl, 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.
2013SoPh..285..317W    Altcode:
  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 Möstl 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° 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.

---------------------------------------------------------
Title: The analysis of polar jet responses using images from the
    LASCO C2 and STEREO COR 2 coronagraphs
Authors: Yu, H. -S.; Jackson, B. V.; Clover, J. M.; Buffington, A.
2013AIPC.1539...90Y    Altcode:
  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.

---------------------------------------------------------
Title: Heliospheric Solar Wind Forecasting Using Observations of
    Interplanetary Scintillation (IPS)
Authors: Jackson, Bernard V.; Yu, Hsiu-Shan; Hick, Paul; Buffington,
   Andrew; Mejia-Ambriz, Julio; Luckett, Nolan; Bisi, Mario
2013shin.confE..86J    Altcode:
  At the University of California, San Diego (UCSD), remote-sensing
  analyses of the inner heliosphere have been regularly carried
  out using radio interplanetary scintillation (IPS) data for
  almost two decades. These analyses have measured and reconstructed
  three-dimensional (3D) solar wind structure throughout this time period
  where data have been available. These global results, especially using
  the Solar-Terrestrial Environment Laboratory (STELab) IPS arrays,
  provide a forecast of solar wind parameters and a time-dependent
  inner boundary in 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 IPS velocity analyses we can
  accurately convect outwards the solar surface magnetic fields and thus
  can provide values of the field (radial and tangential components)
  throughout the global volume. In the inner heliosphere the results
  of these 3D analyses of density, velocity, and vector magnetic field
  have been forecast and compared successfully with in-situ measurements
  obtained near Earth, STEREO, Mars, Venus, MESSENGER, and at the Ulysses
  spacecraft. The resulting precise time-dependent measurements are
  also used to provide an inner boundary of these parameters that can
  be further extrapolated outward to the edge of the heliosphere using
  current 3D-MHD modeling techniques.

---------------------------------------------------------
Title: Using comet plasma tails to study the solar wind
Authors: Jackson, B. V.; Buffington, A.; Clover, J. M.; Hick, P. P.;
   Yu, H. -S.; Bisi, M. M.
2013AIPC.1539..364J    Altcode:
  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.

---------------------------------------------------------
Title: Are Jets CMEs?
Authors: YU, HSIU-SHAN; Jackson, Bernard V.; Buffington, Andrew;
   Hick, P. Paul
2013shin.confE.165Y    Altcode:
  The brightest jets observed by the Hinode XRT and the SDO/AIA
  spacecraft instrumentation produce high-speed responses and enhanced
  brightness that can be traced through coronagraph images and into the
  heliosphere. Specifically, LASCO C2 and STEREO COR2 coronagraph images
  measure the coronal responses to some of the largest jets, and analyses
  using velocities from interplanetary scintillation (IPS) observations
  and the Solar Mass Ejection Imager (SMEI) 3D reconstructions measure
  these jet responses in the heliosphere. We determine the approximate
  masses and energies for these large jet responses over polar coronal
  hole regions, and relate them to the jet peak brightness spectrum
  observed by Hinode during a three-week survey period in September
  2007. We find in our analyses that jets contribute about 5% of the
  total solar wind mass during this period. Assuming that a continuous
  material outflow is associated with jets globally throughout the solar
  cycle, jet responses provide a contribution of mass equivalent to CMEs
  to the solar wind.

---------------------------------------------------------
Title: Heliospheric Solar Wind Parameter Forecasting Using
    Interplanetary Scintillation (IPS) Observations
Authors: Jackson, B. V.; Hick, P.; Buffington, A.; Yu, H.;
   Mejia-Ambriz, J. C.; Luckett, N.; Bisi, M. M.
2013AGUSMSH42B..02J    Altcode:
  At the University of California, San Diego (UCSD), remote-sensing
  analyses of the inner heliosphere have been regularly carried out using
  radio interplanetary scintillation (IPS) data for almost two decades
  employing data from the Solar-Terrestrial Environment Laboratory
  (STELab), Japan, IPS arrays. More recently, several other world
  locations have planned to join in this effort in order to provide
  more complete coverage at times other than those above the celestial
  meridian of the observing station. These analyses have measured and
  reconstructed three-dimensional (3D) solar wind structure throughout the
  time period when data are available. This enables a real-time forecast
  of solar wind density and velocity outward from the observations that
  is nearly complete over the whole heliosphere with a time cadence of
  about one day. When using the IPS velocity analyses, we can accurately
  convect outwards the solar surface background magnetic fields and thus
  can provide values of the field (radial and tangential components)
  throughout the global volume. In the inner heliosphere the results
  of these 3D analyses of density, velocity, and vector magnetic field
  have been forecast and compared successfully with in-situ measurements
  obtained near Earth, at STEREO, at Mars, at Venus, at MESSENGER, and
  at the Ulysses spacecraft. The resulting precise time-dependent results
  can also be used to provide an inner boundary of these parameters that
  can be further extrapolated outward to the edge of the heliosphere
  using current 3D-MHD modeling techniques.

---------------------------------------------------------
Title: Polar Jet Manifestation in the Inner Heliosphere from Images
    using the LASCO C2 and STEREO COR2 Coronagraphs and 3D Tomographic
    Reconstructions from Interplanetary Scintillation and the Solar Mass
    Ejection Imager (SMEI)
Authors: Yu, H.; Jackson, B. V.; Buffington, A.
2013AGUSMSH51A..01Y    Altcode:
  The brightest of the polar jets observed by the Hinode XRT and
  the SDO/AIA show a positive correlation with high-speed responses
  traced through coronagraph observations, and into the interplanetary
  medium. LASCO C2 and STEREO COR2 coronagraph images allow measurement of
  the coronal response to some of these jets, and the nearby background
  solar wind velocity giving a determination of their speeds that we
  compare with Hinode and AIA observations. By using the full data set
  from white light SMEI images, and IPS velocities, we are able to track
  some of these same high speed solar jet responses into the inner
  heliosphere in order to determine the extent to which they retain
  their identity at large solar distances. In this analysis we attempt
  to show the extent with which these individual fast jet responses add
  to the background solar wind.

---------------------------------------------------------
Title: Remote Sensing of Solar Wind Velocities using Interplanetary
    Scintillation with MEXART and STELab Stations
Authors: Mejia-Ambriz, J. C.; Jackson, B. V.; Gonzalez-Esparza, A.;
   Tokumaru, M.; Yu, H.; Buffington, A.; Hick, P.
2013AGUSMSH52A..06M    Altcode:
  Radio signals from compact radio sources are scattered by electron
  density irregularities in the solar wind. This effect is registered
  by radio telescopes as intensity fluctuations of the observed
  radio source amplitude and known as Interplanetary Scintillation
  (IPS). The Mexican Array Radio Telescope (MEXART) and the antennas
  of Solar Terrestrial Environment Laboratory (STELab) are instruments
  dedicated to studies of IPS signals. In this work we present a technique
  (Manoharan and Ananthakrishnan, 1990) used to estimate solar wind
  velocities applied to observations of MEXART and STELab using single
  station spectra. Currently STELab uses a multi-station IPS technique to
  determinate solar wind speeds. Here we compare velocities obtained with
  a single station to those obtained using the multi-station technique
  for a few strong radio sources using both techniques and with both
  instruments. At the Center for Astrophysics and Space Sciences -
  University of California, San Diego (CASS-UCSD), a tomography program
  is able to reconstruct the dynamics of the inner heliosphere globally
  using IPS measurements to give solar wind densities and velocities. We
  show the incorporation of velocities provided by MEXART into this
  program that has been used successfully for over a decade with STELab
  IPS measurements.

---------------------------------------------------------
Title: Tracing Polar Jets into the Inner Heliosphere by Using Images
    from the LASCO C2 and STEREO COR2 Coronagraphs and 3D Tomographic
    Reconstructions from Interplanetary Scintillation and the Solar Mass
    Ejection Imager (SMEI)
Authors: Yu, H.; Jackson, B. V.; Buffington, A.
2012AGUFMSH54A..02Y    Altcode:
  During recent years coordinated efforts to gather data from a large
  number of spacecraft (Hinode, SDO, SOHO, STEREO, and SMEI) and
  ground-based instruments using interplanetary scintillation (IPS),
  have allowed a study of the polar jetting process, and tracing the jet
  response into the heliosphere in a statistical manner. The brightest
  of these polar jets observed by the Hinode XRT and the SDO/AIA show
  a positive correlation with high-speed responses traced into the
  interplanetary medium. LASCO C2 and STEREO COR2 coronagraph images
  allow measurement 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 compare with Hinode and AIA
  observations. By using the full data set from white light SMEI images,
  and IPS velocities, we are able to track these same high speed solar
  jet responses into the inner heliosphere in order to determine the
  extent to which they retain their identity at large solar distances.

---------------------------------------------------------
Title: The Ability of Radio Heliospheric Remote Sensing Observations
    to Provide Global Solar Wind Parameters
Authors: Jackson, B. V.; Hick, P. P.; Buffington, A.; Yu, H.; Bisi,
   M. M.; Fallows, R.
2012AGUFMSH41E..05J    Altcode:
  Heliospheric remote sensing, in particular those using Interplanetary
  Scintillation (IPS) observations, allow the 3-D reconstruction of solar
  wind parameters globally. These parameters include velocity, density,
  and by extrapolation from solar surface magnetogram observations, vector
  magnetic field components. Since the year 2000, the Solar-Terrestrial
  Environment Laboratory (STELab), Nagoya University, Japan, has provided
  a source of IPS data with short-enough latency to enable forecasts of
  these solar wind parameters throughout the inner heliosphere. Over time
  these techniques have been improved upon with data from other radio
  sites (Ootacamund - Ooty - India; and the European Incoherent SCATter
  - EISCAT - radio telescopes based across Northern Scandinavia). Here
  we review the improvements, limitations, and the potential future of
  these techniques. In particular in one new development, the ability to
  measure polarization from radio sources allows the possibility to use
  Faraday rotation inputs to reconstruct heliospheric vector magnetic
  fields without a reliance on solar surface magnetic field extrapolation.

---------------------------------------------------------
Title: 3-D Reconstruction of the Inner Heliosphere From Remote-Sensing
Data: A Global Solar Wind Boundary that Includes CME Transient Effects
Authors: Jackson, B. V.; Yu, H.; Hick, P. P.; Buffington, A.
2012AGUFMSH43C..04J    Altcode:
  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 3-D
  solar wind structure throughout this time period. These global results,
  especially using Solar-Terrestrial Environment Laboratory (STELab)
  IPS observations, provide a time-dependent inner boundary in 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 IPS velocity analyses we can accurately convect-outward
  solar surface magnetic fields and thus provide values of the field
  throughout the global volume. In the inner heliosphere results of these
  3-D analyses of density, velocity, and vector magnetic field have been
  compared successfully with in-situ measurements obtained near Earth,
  STEREO, Mars, Venus, MESSENGER, and at the Ulysses spacecraft. The
  resulting precise time-dependent inner boundary of these parameters
  can be further extrapolated outward to the edge of the heliosphere
  using current 3-D MHD modelling techniques. Here we present sample
  determinations of this boundary for recent IPS data, and give the
  details that allow the interpolation of these boundary values during IPS
  "outage" periods when insufficient remote-sensing data are available
  to provide complete daily coverage.

---------------------------------------------------------
Title: The 3d Analysis of the Heliosphere Using Interplanetary
    Scintillation and Thomson-Scattering Observations
Authors: Jackson, B. V.
2012aogs...30...69J    Altcode: 2012agos...30...69J
  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.

---------------------------------------------------------
Title: Forecasting Transient Heliospheric Solar Wind Parameters at
    the Locations of the Inner Planets
Authors: Jackson, B. V.; Hick, P. P.; Buffington, A.; Clover, J. M.;
   Tokumaru, M.
2012aogs...30...93J    Altcode: 2012agos...30...93J
  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.

---------------------------------------------------------
Title: Modeling Heliosheath Flow with Observational Boundary
    Conditions
Authors: Pogorelov, Nikolai; Wu, ShiTsan; Linker, Jon; Zank, Gary;
   Borovikov, Sergei; Jackson, Bernard; Ebert, Robert; Kim, Tae
2012cosp...39.1517P    Altcode: 2012cosp.meet.1517P
  No abstract at ADS

---------------------------------------------------------
Title: The 3d Reconstructed Global Solar Wind Boundary from
    Remote-Sensing IPS Data
Authors: Yu, Hsiu-Shan; Jackson, B. V.; Hick, P. P.; Buffington, A.;
   Clover, J. M.; Tokumaru, Munetoshi
2012shin.confE..32Y    Altcode:
  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 a time-dependent inner boundary in
  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 provided by UCSD time-dependent
  tomography, we can accurately convect-outward solar surface magnetic
  fields and thus provide values of the magnetic field throughout the
  global volume. These resulting time-dependent 3D reconstructed results
  of density, velocity, and vector magnetic field, which are available
  from 15 solar radii out to 3.0 AU, have been compared successfully
  with in-situ measurements obtained near Earth, STEREO, Mars, Venus,
  MESSENGER, and at the Ulysses spacecraft. Here we present sample
  determinations of these global solar wind boundary for 3D-MHD models
  from recent IPS data.

---------------------------------------------------------
Title: The 3d Global Forecast of Inner Heliosphere Solar Wind
    Parameters from Remotely-Sensed IPS Data
Authors: Jackson, B. V.; Clover, J. M.; Hick, P. P.; Yu, Hsiu-Shan;
   Buffington, A.; Tokumaru, Munetoshi
2012shin.confE..15J    Altcode:
  At UCSD, remote-sensing forecast analyses of the inner heliosphere
  have been regularly carried out using interplanetary scintillation
  (IPS) data. These analyses have measured and reconstructed the
  3-D time-dependent solar wind structure for almost two decades
  using Solar-Terrestrial Environment Laboratory (STELab) IPS
  observations. More recently we have provided an even more accurate
  3-D forecast analyses by incorporating in-situ spacecraft measurements
  into the remotely-sensed volumes. When using the IPS velocity analyses
  we can accurately convect-outward solar surface magnetic fields using
  potential field model techniques, and thus also provide values of the
  field throughout the global volume. This forecast analysis is being
  operated in real time at the UCSD website http://ips.ucsd.edu, and at
  the NASA Goddard Community Coordinated Modeling Center (CCMC) website:
  http://iswa.ccmc.gsfc.nasa.gov:8080/IswaSystemWebApp/index.jsp? The
  results of these time-dependent 3-D analyses of density, velocity,
  and vector magnetic field are compared with in-situ measurements
  obtained in real time near Earth, and are also displayed in real time
  at all the other inner planets: Mercury, Venus and Mars as well as
  at the locations of the STEREO A and B spacecraft. We display these
  forecasts obtained from our UCSD website at this poster presentation,
  and discuss a metric that we have devised to determine how well these
  forecasts agree with ongoing in-situ measurements.

---------------------------------------------------------
Title: An Analysis of the Origin and Propagation of the Multiple
    Coronal Mass Ejections of 2010 August 1
Authors: Harrison, R. A.; Davies, J. A.; Möstl, 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.
2012ApJ...750...45H    Altcode:
  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.

---------------------------------------------------------
Title: Variable Stellar Object Detection and Light Curves from the
    Solar Mass Ejection Imager (SMEI)
Authors: Hounsell, R. A.; Bode, M. F.; Darnley, M. J.; Harman, D. J.;
   Hick, P. P.; Buffington, A.; Jackson, B. V.; Clover, J. M.; Shafter,
   A. W.
2012IAUS..285...91H    Altcode:
  With the advent of surveys such as the Catalina Real-Time Transient
  Survey, the Palomar Transient Factory, Pan-STARRS and Gaia,
  the search for variable objects and transient events is rapidly
  accelerating. There are, however important existing data-sets from
  instruments not originally designed to find such events. One example
  of such an instrument is the Solar Mass Ejection Imager (SMEI), an
  all-sky space-based differential photometer which is able to produce
  light curves of bright objects (m &lt;= 8) with a 102-minute cadence. In
  this paper we discuss the use of such an instrument for investigations
  of novæ, and outline future plans to find other variable objects with
  this hitherto untapped resource.

---------------------------------------------------------
Title: The 3D Analysis of Polar Jets Using Thomson-Scattering
    Observations from LASCO C3 Images and the Solar Mass Ejection Imager
    (SMEI)
Authors: Yu, H. S.; Jackson, B. V.
2012decs.confE..11Y    Altcode:
  The X-Ray Telescope (XRT) onboard Hinode provides an opportunity to
  observe solar jetting activity above the solar poles. LASCO C3 images
  allow measurements of the coronal response to some of these jets, giving
  a determination of their speeds and energies that we compare with Hinode
  observations (Sako et al. 2010, 38th COSPAR). By using the full SMEI
  (Solar Mass Ejection Imager) image data set, we are able to study these
  same solar jet responses in the inner heliosphere. Preliminary results
  from 3D-reconstructed SMEI pseudo C3 coronagraph images have shown a
  good agreement at the correct position angles and time with the jet
  responses observed in LASCO (Jackson, 2012, Adv. in Geosciences). Using
  the SMEI volumetric data we carry this analysis farther, attempting
  to determine the extent to which these 3D jet responses maintain their
  identity into the inner heliosphere.

---------------------------------------------------------
Title: Necessity of 2D image data for determining 3D configurations
    of magnetic clouds
Authors: Marubashi, K.; Tokumaru, M.; Jackson, B. V.; Clover, J. M.
2011AGUFMSH21A1911M    Altcode:
  The structure of magnetic cloud (MC) has long been studied by
  fitting in-situ magnetic field measurements to magnetic flux rope
  models. Such studies generally provide the size and orientation of the
  model structure, which are taken to be applicable only locally to the
  portion where the cloud passed the spacecraft. The obtained geometry
  often changes depending on the models used for the fitting. For example,
  for a single observational data set, a cylinder model and a torus model
  often give different cloud axis orientations. Thus we need further
  consideration about the global configuration to deduce the 3D structure
  of the MC. 2D images from heliospheric remote sensing measurements
  provide reliable constraints about the global MC structure. With
  the above in mind we attempt to study the global structure of MC by
  combining the model fitting results and the 3D reconstruction data from
  the Solar Mass Ejection Imager (SMEI) and interplanetary scintillations
  (IPS). For this purpose, we first select MC events in which the proton
  densities are high enough (generally &gt; 20 /cc) in the sheath regions
  behind the driven shocks and/or in the regions occupied by MCs. Then
  we examine possible 3D configurations which are consistent with the
  orientation of the MC axis obtained from model fittings. The global MC
  structure is finally obtained by applying the constraints from 2D image
  data. Our preliminary examination shows that the above procedure is
  helpful for determining the most probable 3D global structures of MCs.

---------------------------------------------------------
Title: Comparative Validation of Realtime Solar Wind Forecasting
    Using the UCSD Heliospheric Tomography Model
Authors: MacNeice, P. J.; Taktakishvili, A.; Jackson, B. V.; Clover,
   J. M.; Bisi, M. M.; Odstrcil, D.
2011AGUFMSH31C2026M    Altcode:
  The University of California, San Diego 3D Heliospheric Tomography
  Model reconstructs the evolution of heliospheric structures, and can
  make forecasts of solar wind density and velocity up to 72 hours in
  the future. The latest model version, installed and running in near
  real-time at the Community Coordinated Modeling Center(CCMC), analyzes
  scintillations of meter wavelength radio point sources recorded by
  the Solar-Terrestrial Environment Laboratory (STELab) together with
  real-time measurements of solar wind speed and density recorded by
  the Advanced Composition Explorer(ACE) Solar Wind Electron Proton
  Alpha Monitor(SWEPAM). The solution is reconstructed using tomographic
  techniques and a simple kinematic wind model. Since installation, the
  CCMC has been recording the model forecasts and comparing them with
  ACE measurements, and with forecasts made using other heliospheric
  models hosted by the CCMC. We report the preliminary results of this
  validation work and comparison with alternative models.

---------------------------------------------------------
Title: A Snapshot of the Sun Near Solar Minimum: The Whole Heliosphere
    Interval
Authors: Thompson, Barbara J.; Gibson, Sarah E.; Schroeder, Peter C.;
   Webb, David F.; Arge, Charles N.; Bisi, Mario M.; de Toma, Giuliana;
   Emery, Barbara A.; Galvin, Antoinette B.; Haber, Deborah A.; Jackson,
   Bernard V.; Jensen, Elizabeth A.; Leamon, Robert J.; Lei, Jiuhou;
   Manoharan, Periasamy K.; Mays, M. Leila; McIntosh, Patrick S.; Petrie,
   Gordon J. D.; Plunkett, Simon P.; Qian, Liying; Riley, Peter; Suess,
   Steven T.; Tokumaru, Munetoshi; Welsch, Brian T.; Woods, Thomas N.
2011SoPh..274...29T    Altcode: 2011SoPh..tmp..413T
  We present an overview of the data and models collected for the
  Whole Heliosphere Interval, an international campaign to study the
  three-dimensional solar-heliospheric-planetary connected system near
  solar minimum. The data and models correspond to solar Carrington
  Rotation 2068 (20 March - 16 April 2008) extending from below the
  solar photosphere, through interplanetary space, and down to Earth's
  mesosphere. Nearly 200 people participated in aspects of WHI studies,
  analyzing and interpreting data from nearly 100 instruments and
  models in order to elucidate the physics of fundamental heliophysical
  processes. The solar and inner heliospheric data showed structure
  consistent with the declining phase of the solar cycle. A closely
  spaced cluster of low-latitude active regions was responsible for an
  increased level of magnetic activity, while a highly warped current
  sheet dominated heliospheric structure. The geospace data revealed an
  unusually high level of activity, driven primarily by the periodic
  impingement of high-speed streams. The WHI studies traced the solar
  activity and structure into the heliosphere and geospace, and provided
  new insight into the nature of the interconnected heliophysical system
  near solar minimum.

---------------------------------------------------------
Title: A Study of Long-Term Heliospheric Brightness Using SMEI Data
Authors: Buffington, A.; Clover, J. M.; Hick, P. P.; Jackson, B. V.;
   Bisi, M. M.
2011AGUFMSH13B1970B    Altcode:
  The Solar Mass Ejection Imager (SMEI) has been returning white-light
  photometric maps of nearly the entire sky with a 102-minute cadence
  for well over eight years. When the usual sidereal and zodiacal
  backgrounds are removed, the residual maps are used to study
  CME/ICME events. Moreover, the successful sidereal subtraction
  provides a certification of SMEI's photometric accuracy over this
  time period. Further, since the zodiacal background removal employs a
  brightness model which does not vary with time, a search for potential
  long-term changes in the residue can show whether the zodiacal cloud's
  dust distribution varies within this portion of the present solar
  cycle. We present results from studies using SMEI imagery along with
  a concluded zodiacal-light model.

---------------------------------------------------------
Title: SMEI and IPS 3-D CME Reconstructions, and What They Indicate
    of Heliospheric Solar Wind Acceleration
Authors: Jackson, B. V.; Clover, J. M.; Hick, P. P.; Buffington, A.;
   Bisi, M. M.; Tokumaru, M.
2011AGUFMSH32A..05J    Altcode:
  The remotely-sensed measurements of coronal mass ejections (CMEs) and
  their interplanetary counterparts (ICMEs) from Solar Mass Ejection
  Imager (SMEI) white-light brightness and radio interplanetary
  scintillation (IPS) data can be used to provide limits on the
  acceleration and deceleration of transients in the inner heliosphere. As
  an intermediate measurement between the Sun and 1 AU, the limits
  provided by remote sensing are convolved with line-of-sight effects and
  CME/ICME `evolution' as each feature of the transient moves outward
  from the Sun. Here we review a few of the popular events and studies
  that have been presented to show how CME propagation proceeds in the
  inner heliosphere. Often, the apparent acceleration shown can only be
  provided by employing an assumption of the CME three-dimensional (3-D)
  shape, which often changes with solar distance and CME visibility along
  the line of sight. This assumption can often abrogate the original
  acceleration measurement. In particular we concentrate here on the
  analysis of two events during periods in 02-04 November 2003, and
  also in January 2010 showing how each event provides significantly
  different acceleration profiles depending on which structures are
  identified in each transient. Finally, we highlight the strange case
  of polar coronal jets (that are essentially miniature CMEs) frequently
  observed to move outward in the polar coronal fast wind at speeds of
  over three times ambient. These small solar wind transients seem to
  have disappeared by the time they can be observed in Ulysses in-situ
  data. Thus, a detailed study of these jets may provide an understanding
  of smaller-scale CME/ICME deceleration processes.

---------------------------------------------------------
Title: UCSD Time-Dependent Tomographic Forecasting with Interplanetary
    Scintillation and White-Light Observations
Authors: Clover, J. M.; Jackson, B. V.; Hick, P. P.; Buffington, A.;
   Tokumaru, M.; Fujiki, K.; Hirota, M.; Bisi, M. M.
2011AGUFMSH31C2025C    Altcode:
  The University of California, San Diego (UCSD) time-dependent tomography
  program has been used successfully since the beginning of the year
  2000 to remotely sense and forecast interplanetary scintillation (IPS)
  observations of coronal mass ejections (CMEs). Recently, this program
  has included real-time ACE data in the analysis. This more-efficiently
  extends velocity and density measurements obtained near Earth in
  real time to those derived from remotely-sensed observations, and
  allows a far more efficient extrapolation from the present time
  into the future. These analyses are now also used with real-time
  extrapolations of radial and tangential magnetic fields from the
  National Solar Observatory. The time-dependent program is also being
  adapted to provide similar forecasts (but at higher spatial and temporal
  resolutions) of heliospheric density using Thomson-scattering data from
  the Solar Mass Ejection Imager (SMEI). Here, we describe the current
  state of these IPS and SMEI real-time data pipelines and show their
  usefulness. These demonstrate in near real-time the improved accuracy
  of the remote-sensing fits with the inclusion of space-borne in-situ
  density and velocity measurements during the current rising phase of
  the solar cycle.

---------------------------------------------------------
Title: Imaging Coronal Mass Ejections and Large-Scale Solar Wind
    Structure Using Thomson-Scattering Measurements from SMEI
Authors: Jackson, B. V.; Clover, J. M.; Buffington, A.; Hick, P. P.;
   Bisi, M. M.; Marubashi, K.; Webb, D. F.
2011AGUFMSH21A1909J    Altcode:
  In January 2010, two coronal mass ejections (CMEs) erupted from near
  the solar east limb, the first on late 14 January 2010 and the second
  on 17 January 2010. Both arrived at the Solar TErrestrial RElations
  Observatory Behind spacecraft (STEREO-B) about six days later. We are
  able to reconstruct the heliospheric density of both CME events in
  three dimensions (3D) using data from the Solar Mass Ejection Imager
  (SMEI) and our tomographic analysis. For each event, we isolate the
  particular portion of the heliosphere attributed to the transient
  CME density structure from the tomographic results, and then estimate
  its extent. The structure of these events is shown in detail in the
  three-dimensional reconstruction both as pseudo-coronagraph images
  and later as density at the locations of STEREO-B and the Earth. The
  first of these CMEs was associated with a magnetic cloud that had a
  density enhancement near its center. By assuming that this density
  enhancement extends along the loop, we can use the three-dimensional
  density analysis to map the extent and orientation of this structure
  in order to match it to existing magnetic-loop models and to use the
  remote-sensing observations to constrain the various flux-rope models
  determined using the in-situ measurements of the 14 January 2010 event.

---------------------------------------------------------
Title: Current and Planned Solar Wind Observations Using the EISCAT
    and LOFAR Radio-Telescope Systems
Authors: Bisi, M. M.; Fallows, R. A.; Jensen, E. A.; Breen, A.; Xiong,
   M.; Jackson, B. V.
2011AGUFMSH31C2020B    Altcode:
  Remote-sensing observations of the inner heliosphere using the technique
  of interplanetary scintillation (IPS) provide essential information
  on the velocity and density of developing solar wind structure. For
  many years, observations of IPS have been undertaken with the European
  Incoherent SCATter (EISCAT) radio telescopes based across Northern
  Scandinavia. We are presently developing the IPS experiment for use on
  new and upcoming cutting-edge instrumentation. Such instrumentation
  includes the LOw Frequency ARray (LOFAR) which is situated primarily
  in the Netherlands with additional stations currently sited across
  central Europe. Using data sets from various IPS-capable systems,
  the University of California, San Diego (UCSD) three-dimensional
  (3-D) tomographic-reconstruction and visualisation algorithms
  can yield reconstruction results for comparison with multi-point
  it{in-situ} measurements from spacecraft. This makes it possible to
  study the structure of the inner heliosphere as a whole, including
  the isolation of individual features or events such as interplanetary
  coronal mass ejections (ICMEs), stream interaction regions (SIRs), or
  their interactions with the ambient solar wind as well as the ambient
  wind itself. We are also testing the Faraday rotation (FR) response
  at low frequencies using LOFAR. Combined, these techniques have large
  implications and capabilities for space-weather forecasting. This work
  is focused on the global structure of the inner heliosphere during
  the minimum and rise phases of the current solar cycle.

---------------------------------------------------------
Title: Using Global Heliospheric Reconstructions to Separate Multiple
    CME and CIR Flows
Authors: Webb, D. F.; Jackson, B. V.; Bisi, M. M.; Howard, T. A.
2011AGUFMSH31C2024W    Altcode:
  The heliospheric propagation of density structures has been observed and
  measured by the heliospheric imagers (HIs) of the Solar Mass Ejection
  Imager (SMEI) in Earth orbit since early 2003 and on the twin Solar
  TErrestrial RElations Observatory (STEREO) spacecraft in ~1 AU solar
  orbits since early 2007. We discuss several three-dimensional (3-D)
  reconstruction techniques being used with these HI data sets and their
  capabilities for distinguishing and tracking separate CME/ICME flows
  in the inner heliosphere during very active periods, and/or separating
  CME/ICME and CIR flows. We include heliospheric modeling techniques
  based on kinematical solar wind models, MHD models, and the empirical
  Tappin-Howard (T-H) model. We focus on two periods of high activity:
  January 2010 and July-August 2010. We will also look at events during
  the Whole Heliosphere Interval (WHI) Campaign in March-April 2008.

---------------------------------------------------------
Title: Propagation and impact of multiple coronal mass ejections
    events on August 1 2010 in the heliosphere
Authors: Möstl, Christian; Farrugia, Charles J.; Harrison, Richard
   A.; Davies, J. A.; Kilpua, Emilia K. J.; Odstrcil, Dusan; Rollett,
   Tanja; Temmer, Manuela; Veronig, Astrid; Jian, Lan; Liu, Ying;
   Eastwood, Jonathan; Forsyth, Robert; Webb, David; Bisi, Mario M.;
   Jackson, Bernard V.; Mulligan, Tamitha; Jensen, Liz; Lavraud, Benoit;
   de Koning, Curt A.; Nitta, Nariaki; Luhmann, Janet; Galvin, Antoinette
   B.; Zhang, Tielong
2011sdmi.confE..69M    Altcode:
  On August 1 2010 a large region of the solar northern hemisphere
  displayed major activity involving a complex set of central meridian and
  remote active regions, and two large prominence channels (Schrijver
  and Title, JGR, 2011). We witnessed the eruption of four coronal
  mass ejections (CMEs) which partly impacted Earth and lead to one
  of the first geomagnetic storms of the new solar cycle. We present an
  overview of the results of several analyses exploiting the extraordinary
  completeness of the imaging data (SDO/STEREO/SOHO) in combination with
  numerical simulations (ENLIL) and in situ observations. The imprints of
  the CMEs, including a prior event on July 30, were observed in situ in
  an almost laboratory-like configuration at 4 widely separated locations
  spanning over 120 degrees of heliospheric longitude (STEREO-B, Venus
  Express, ACE/Wind, ARTEMIS, and MESSENGER). The CME density enhancements
  could be followed with the STEREO-A/HI and Coriolis/SMEI instruments
  continuously from the Sun to 1 AU. Evidences of CME-CME interactions
  and resulting overlapping tracks in Jmaps make the analysis complex,
  but nevertheless we find robust interpretations for linking two magnetic
  flux ropes at Earth, one of them geo-effective and including elevated
  alpha particles related to possible filament material, to their solar
  counterparts. Additionally, we discuss the relationship between the
  in situ observations and the global picture given by the ENLIL model.

---------------------------------------------------------
Title: Observations of Polar-Region Jets and Their Manifestations
    in the Solar Wind
Authors: Jackson, Bernard V.; Clover, John M.; Hick, P. Paul;
   Buffington, Andrew; Linford, John C.; Shimojo, Masumi; Sako, Nobuharu
2011shin.confE.170J    Altcode:
  High-cadence images taken by the X-Ray Telescope (XRT) aboard Hinode
  (Solar B), have shown that X-ray jets occur at very high frequency over
  the polar regions of the Sun. Only the brightest of these explosive
  events had been previously observed. It is possible that Alfven waves
  generated by jets contribute greatly to the acceleration of the solar
  wind; each jet provides a conduit for Alfven waves that add significant
  energy to the corona by spreading outward from these localized areas
  on the Sun. Here we explore the manifestations of the jet response in
  the solar wind using observations from Hinode, the LASCO coronagraph,
  and from 3D tomographic observations at greater heights above the
  Sun. We attempt to quantify the jet response in the interplanetary
  medium from these measurements, and to explore the diminution of this
  response with solar radius.

---------------------------------------------------------
Title: UCSD Time-Dependent Tomographic Forecasting with Interplanetary
    Scintillation and White Light Observations
Authors: Clover, John M.; Jackson, Bernard V.; Hick, P. Paul;
   Buffington, Andrew; Lindford, John C.
2011shin.confE..20C    Altcode:
  The University of California, San Diego (UCSD) time-dependent tomography
  program has been used successfully since the beginning of the year
  2000 to remotely sense and forecast interplanetary scintillation (IPS)
  observations of coronal mass ejections. Recently, this program has
  incorporated ACE data in the analysis to more efficiently extend,
  in real time, near-Earth observations of velocity and density, to
  those derived from remotely-sensed observations. This allows a more
  efficient extrapolation from the present time into the future. The
  time-dependent program has now also been adapted to provide forecasts
  of heliospheric density using Thomson-scattered brightness from the
  Solar Mass Ejection Imager (SMEI). Here we describe the current state
  of these IPS and SMEI real-time data pipelines, and show examples of
  the improved accuracy of the remote-sensing fits with the inclusion
  of space-borne in-situ density and velocity measurements.

---------------------------------------------------------
Title: Solar Mass Ejection Imager (SMEI) 3-D reconstruction of density
enhancements behind interplanetary shocks: In-situ comparison near
    Earth and at STEREO
Authors: Jackson, B. V.; Hamilton, M. S.; Hick, P. P.; Buffington,
   A.; Bisi, M. M.; Clover, J. M.; Tokumaru, M.; Fujiki, K.
2011JASTP..73.1317J    Altcode:
  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 L<SUB>1</SUB>
  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 L<SUB>1</SUB>.

---------------------------------------------------------
Title: Investigations of the July-August 2010 CME Event(s)
Authors: Bisi, Mario M.; Jackson, Bernard V.; Clover, John M.; Jensen,
   Elizabeth A.; Mulligan, Tamitha M.; Manoharan, Periasamy K.; Hick,
   P. Paul
2011shin.confE.130B    Altcode:
  A complex solar eruption (or set of eruptions) occurred at the start
  of August 2010 releasing a disappearing filament and halo CME on an
  Earth-wards trajectory launching from AR 1092. The first ICME arrived on
  03 August followed by a second stronger ICME on 04; both were travelling
  at speeds approximately twice that of the ambient solar wind of the
  time. The ICMEs triggered a G2-class geomagnetic storm. Here, we look
  at the 3-D reconstruction of the event(s) from Solar Mass Ejection
  Imager (SMEI) white-light data, and where possible, interplanetary
  scintillation (IPS) data. We also discuss flux-rope modelling results
  as measured by ACE, VEX, and STEREO-B instrumentation. We will discuss
  and attempt to pull together our findings in the context of the inner
  heliosphere.

---------------------------------------------------------
Title: Three-dimensional reconstruction of heliospheric structure
using iterative tomography: A review
Authors: Jackson, B. V.; Hick, P. P.; Buffington, A.; Bisi, M. M.;
   Clover, J. M.; Tokumaru, M.; Kojima, M.; Fujiki, K.
2011JASTP..73.1214J    Altcode:
  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 R<SUB>S</SUB>). 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.

---------------------------------------------------------
Title: The early outburst light curve of the 2011 eruption of the
    Recurrent Nova T Pyxidis from Solar Mass Ejection Imager (SMEI)
    observations
Authors: Hounsell, R.; Darnley, M. J.; Harman, D. J.; Bode, M. F.;
   Clover, J. M.; Hick, P. P.; Buffington, A.; Jackson, B. V.; Osborne,
   J.; Shafter, A. W.
2011ATel.3373....1H    Altcode:
  We report white light observations of the 2011 outburst of
  Recurrent Nova T Pyxidis obtained using the USAF/NASA Solar Mass
  Ejection Imager (SMEI) on board the Coriolis satellite (see <A
  href="http://adsabs.harvard.edu/abs/2010ApJ...724..480H">Hounsell
  et al., 2010</A> for details, all magnitudes quoted here are native
  to the SMEI photometric system). The instrument has a peak quantum
  efficiency at approximately 700 nm with a FWHM ~ 300 nm.

---------------------------------------------------------
Title: The 3D Reconstruction of Heliospheric Density Using
    Thomson-Scattering Observations - Current Progress and Future
    Prospects
Authors: Jackson, Bernard V.; Clover, J. M.; Buffington, A.; Hick,
   P. P.
2011SPD....42.1401J    Altcode: 2011BAAS..43S.1401J
  Three-dimensional reconstructions using Thomson-scattering observations
  from the Air Force/NASA Solar Mass Ejection Imager (SMEI) provide
  a determination of density in the inner heliosphere and allow its
  forecast from these remote-sensing heliospheric data. Here we describe
  our recent progress in providing density from this technique, and our
  current success in this endeavor. We would like to provide the best
  possible remote determinations of this heliospheric parameter. Here we
  explore this possibility with the copious data available from the SMEI
  imagery that can now be cleaned of auroral signals such that as many
  as 10,000 lines of sight can be available on each 102-minute orbit. We
  speculate on the degree to which these methods and results could be
  used on future heliospheric missions, should such instruments on such
  missions provide images as finely-calibrated as those from SMEI.

---------------------------------------------------------
Title: Outburst of Comet 17P/Holmes Observed with the Solar Mass
    Ejection Imager
Authors: Li, Jing; Jewitt, David; Clover, John M.; Jackson, Bernard V.
2011ApJ...728...31L    Altcode: 2010arXiv1012.1570L
  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 1070 ± 40 km<SUP>2</SUP>
  s<SUP>-1</SUP> while the (model-dependent) mass loss rates inferred
  from the light curve reach a maximum at 3 × 10<SUP>5</SUP> kg
  s<SUP>-1</SUP>. The integrated mass in the coma lies in the range
  (2-90) × 10<SUP>10</SUP> 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.

---------------------------------------------------------
Title: Analysis of Epsilon Aurigae light curve from the Solar Mass
    Ejection Imager
Authors: Clover, John; Jackson, B. V.; Buffington, A.; Hick, P. P.;
   Kloppenborg, B.; Stencel, R.
2011AAS...21725702C    Altcode: 2011BAAS...4325702C
  The Solar Mass Ejection Imager (SMEI) was launched aboard the Coriolis
  spacecraft in 2003. It is equipped with 3 CCD cameras to measure the
  brightness of Thomson-scattered electrons in the heliosphere. Each
  CCD images a strip of the sky that is 3°x60°. The three cameras are
  mounted on the satellite with their fields of view aligned end-to-end
  so that SMEI sweeps nearly the entire sky each 102 minute orbit. SMEI
  has now accumulated stellar time series for about 5700 bright stars,
  including epsilon Aurigae, for each orbit where data is available. SMEI
  data provide nearly year-round coverage of epsilon Aurigae. The baffled
  SMEI optics provide more accurate photometric data than ground-based
  observations, particularly at mid-eclipse when epsilon Aurigae is close
  to the Sun. We present an analysis of the brightness variations of
  the epsilon Aurigae system, before and during the eclipse. <P />The
  University of Denver participants are grateful for support under
  NSFgrant 10-16678 and the bequest of William Hershel Womble in support
  of astronomy at the University of Denver.

---------------------------------------------------------
Title: Solar Mass Ejection Imager (SMEI) 3-D Reconstructions of CMEs,
    CIRs and Interplanetary Shocks, and Comparison with In-situ Data
Authors: Jackson, B. V.; Clover, J. M.; Hick, P. P.; Buffington, A.;
   Bisi, M. M.
2010AGUFMSH31D..05J    Altcode:
  The Solar Mass Ejection Imager (SMEI) has been operating since February
  2003. At the University of California, San Diego (UCSD), a series
  of editing steps and a tomography program removes zodiacal light,
  high-energy-particle hits, and aurorae the SMEI data; and generates
  reconstructed sky-map images and three-dimensional (3-D) volumetric
  densities shortly after the SMEI CCD images become available. The
  removal of a long-term base allows us to map the 3-D density extents of
  coronal mass ejections (CMEs) and co-rotating structures, and measure
  the density variations of these structures including estimates of their
  continuity and the extent of density enhancements behind interplanetary
  shocks. We match our analysis with the in-situ density columns that pass
  the spacecraft near Earth as well as near the twin Solar TErrestrial
  RElations Observatory (STEREO) spacecraft. Here we concentrate on
  Thomson-scattered white-light SMEI observations of the 3 April 2010
  halo CME, contrasting it to the studies of previous CME events that
  provide similar Sun-to-Earth analyses.

---------------------------------------------------------
Title: Remote-Sensing Studies of Heliospheric Solar-Wind Structure
    Around Two Solar Minima
Authors: Bisi, M. M.; Clover, J. M.; Breen, A.; Jensen, E. A.; Fallows,
   R.; Jackson, B. V.; Hick, P. P.; Rawlins, A.; Davies, J. A.; Owens,
   M.; Xiong, M.; Buffington, A.; Grande, M.
2010AGUFMSH41A1771B    Altcode:
  Remote-sensing observations of the inner heliosphere are carried out
  routinely using both the interplanetary scintillation (IPS) observations
  of astronomical radio sources and also the Thomson-scattered white
  light from heliospheric electrons. For these latter observations,
  we use the Earth-orbiting Solar Mass Ejection Imager (SMEI: from
  February 2003) aboard the Coriolis Satellite, and more recently using
  the Heliospheric Imagers (HIs) aboard the Solar TErrestrial RElations
  Observatory twin spacecraft (STEREO: from late 2006/early 2007). The
  data sets from various IPS-capable systems as well as SMEI are used
  with the University of California, San Diego (UCSD) three-dimensional
  (3-D) tomographic-reconstruction and visualisation algorithms. We are
  able to compare with in-situ measurements from multiple spacecraft
  with these reconstruction results. This makes it possible to study the
  structure of the inner heliosphere as a whole, including the isolation
  of individual features or events such as interplanetary coronal mass
  ejections (ICMEs) or stream interaction regions (SIRs). We look at the
  global structure of the heliosphere during the current and previous
  solar minima, and discuss similarities and differences between the
  two solar cycles where possible.

---------------------------------------------------------
Title: Imaging Coronal Mass Ejections and Large-Scale Solar Wind
    Structure Using IPS and Thomson-Scattered Sunlight (Invited)
Authors: Clover, J. M.; Jackson, B. V.; Buffington, A.; Hick, P. P.;
   Bisi, M. M.; Tokumaru, M.; Fujiki, K.
2010AGUFMSH52B..03C    Altcode:
  The Solar Mass Ejection Imager (SMEI) observes Thomson-scattered
  white light from heliospheric electrons across almost all of the sky
  nearly all of the time since early 2003. Interplanetary scintillation
  (IPS) observations of velocity and g-level provide similar structure
  information but with a less-complete sky-and-time coverage. The
  Solar TErrestrial RElations Observatory (STEREO) twin spacecraft
  outer Heliospheric Imagers (HI-2) currently image the heliosphere in
  Thomson-scattered light near the ecliptic plane far from Earth. The
  Solar-Terrestrial Environment Laboratory (STELab) IPS observations
  provide IPS velocity and g-level values, which in conjunction with our
  tomographic reconstruction program, yield velocities and densities
  of the inner heliosphere in three dimensions. The same tomographic
  program substitutes SMEI Thomson-scattering brightness information for
  the g-level values to derive heliospheric densities from these data
  alone. We look at the global structure of the heliosphere concentrating
  mainly on three events from 2007 through the rise phase of Solar Cycle
  24. The first event, observed in both the IPS and SMEI defines the
  three-dimensional velocity and density structure around the time of the
  shock observed at Earth on 02:02 UT 17 December 2007. The second event,
  seen only by SMEI, is that of the 23-26 April 2008 coronal mass ejection
  (CME) and its interplanetary counterpart. The third event is the CME
  (and its interplanetary counterpart) that took place 17 January 2010
  and arrived at STEREO-B about four days later. For each event, we
  isolate the particular portion of the heliosphere attributed to the
  transient density structure using our tomographic technique, and then
  estimate its extent.

---------------------------------------------------------
Title: Type III Metric Radio-Wave Activity Prior to and During Active
    Region Flaring and CMEs (Invited)
Authors: Jackson, B. V.; Hick, P. P.; Buffington, A.; Oberoi, D.;
   Matthews, L. D.
2010AGUFMSH54D..03J    Altcode:
  From the time that type III metric radio-wave activity has been known,
  and imaged, there has been a realization that this activity often
  increases during, and for some events from a few minutes to several
  hours prior to the major manifestations observed for a flare or Coronal
  Mass Ejection (CME). We review these analyses from as long ago as the
  observations from Culgoora, Australia, and more recently from the French
  Nancay radio observatory. We find there can be precursor activity before
  a flare or CME as indicated by the increasing numbers of isolated type
  III bursts, and that this can be a maximum prior to the most obvious
  manifestation of either the surface flare or the most obvious rapid
  outward coronal motion of a CME. Current imaging measurements from the
  Nancay radio array further clarify the location of this activity for
  specific events such as the 26 April 2008 CME that was observed just
  following the Whole Heliosphere Interval (WHI) near the time of solar
  minimum. A plausible explanation for this precursor activity exists,
  and we expect that this idea can be more fully tested using present-day
  observations. As solar activity increases and more observations become
  available from, for instance, the Murchison Widefield Array (MWA) now
  under construction in Western Australia, far better worldwide temporal
  coverage for this type of analysis will exist. In conjunction with
  current NASA instrumentation such as the Solar TErrestrial RElations
  Observatory (STEREO) and SOlar and Heliospheric Observatory (SOHO)
  coronagraphs, and the Solar Dynamics Observatory (SDO), we expect a
  significant improvement in our understanding of this unique flare and
  CME precursor activity.

---------------------------------------------------------
Title: End-to-End Observations and Modeling of the 17-21 January
    2010 CME/ICME
Authors: Webb, D. F.; Cliver, E. W.; Nitta, N. V.; Attrill, G. D.;
   Marubashi, K.; Howard, T. A.; Tappin, J.; Jackson, B. V.
2010AGUFMSH41A1778W    Altcode:
  On 17 January 2010, before it rotated onto the Earth-facing disk and
  produced a series of M-class X-ray flares, active region 11041 was
  associated with an energetic CME with a coronal wave and dimming, radio
  type II and III emission. During launch the CME revealed an unusual
  circular profile viewed from STEREO-B with EUVI and extending into
  the COR1 field. It was also observed over the southeast limb from SOHO
  EIT and LASCO from which it appeared as a partial halo. The views from
  STEREO and SOHO near the Sun and HI-A and SMEI at 1 AU suggest that at
  least part of the CME traveled toward STEREO-B, where a small magnetic
  cloud was observed on 21 January. The importance of this event lies in
  the multiwavelength observations with high time cadences of near-limb
  observations of a CME, its manifestations in the low corona, its passage
  through the heliosphere and its appearance as an ICME/magnetic cloud
  in-situ at STEREO-B 3.5 days later. This event permits us to study the
  origin and driving of the wave because the flanks of the CME and its
  relationship to the wave can be studied in detail. Our interpretation
  is that the wave is initially driven by the CME and then becomes freely
  propagating after the CME lateral expansion ends. Several models are
  used to understand the 3-D geometry and propagation of the CME, and
  two flux rope models are compared with the launch observations and
  magnetic field orientations.

---------------------------------------------------------
Title: SMEI 3D Reconstruction of a Coronal Mass Ejection Interacting
with a Corotating Solar Wind Density Enhancement: The 2008 April
    26 CME
Authors: Jackson, B. V.; Buffington, A.; Hick, P. P.; Clover, J. M.;
   Bisi, M. M.; Webb, D. F.
2010ApJ...724..829J    Altcode:
  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.

---------------------------------------------------------
Title: A Heliospheric Imager for Deep Space: Lessons Learned from
    Helios, SMEI, and STEREO
Authors: Buffington, A.; Jackson, B. V.; Hick, P. P.; Clover, J. M.;
   Bisi, M. M.
2010AGUFMSH41A1780B    Altcode:
  The zodiacal-light photometers on the twin Helios spacecraft, the
  Solar Mass Ejection Imager (SMEI) aboard the Coriolis spacecraft, and
  the Heliospheric Imagers (HIs) on the twin Solar-TErrestrial RElations
  Observatory (STEREO) spacecraft all point the way to optimizing future
  remote-sensing Thomson-scattering observations from deep space. In the
  future, such data could be provided by wide-angle viewing instruments
  deployed on Solar Orbiter, Solar Probe Plus, and other deep-space
  missions. Here, we present instrument specifications required for a
  successful heliospheric imager, and the calibration measurements and
  data-processing steps that enable the best use of these remote-sensing
  systems. When properly designed and calibrated, data from these types
  of instruments measure zodiacal-dust properties, and are used to
  provide three-dimensional reconstructions of heliospheric electron
  density over large volumes of the inner heliosphere. Such systems
  measure fundamental properties of the inner heliospheric plasma,
  provide context for the in-situ monitors on board spacecraft, and
  perhaps most significantly, enable physics-based analyses of this
  important segment of the Sun-Spacecraft connection.

---------------------------------------------------------
Title: Exquisite Nova Light Curves from the Solar Mass Ejection Imager
    (SMEI)
Authors: 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.
2010ApJ...724..480H    Altcode: 2010arXiv1009.1737H
  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.

---------------------------------------------------------
Title: A Summary of 3-D Reconstructions of the Whole Heliosphere
    Interval and Comparison with in-Ecliptic Solar Wind Measurements
    from STEREO, ACE, and Wind Instrumentation
Authors: Bisi, Mario M.; Jackson, B. V.; Clover, J. M.; Hick, P. P.;
   Buffington, A.; Tokumaru, M.
2010HiA....15..480B    Altcode:
  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.

---------------------------------------------------------
Title: Three-Dimensional (3-D) Reconstruction of Solar-Wind Structure
    at the Inner Planets and in the Inner Heliosphere
Authors: Bisi, M. M.; Jackson, B. V.; Wood, A. G.; Clover, J. M.;
   Breen, A. R.; Fallows, R. A.; Jensen, E. A.; Tokumaru, M.; Fujiki,
   K.; Hick, P. P.
2010epsc.conf..882B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Three-Dimensional (3-D) Reconstructions of EISCAT IPS Velocity
    Data in the Declining Phase of Solar Cycle 23
Authors: Bisi, M. M.; Jackson, B. V.; Breen, A. R.; Dorrian, G. D.;
   Fallows, R. A.; Clover, J. M.; Hick, P. P.
2010SoPh..265..233B    Altcode: 2010SoPh..tmp..129B; 2010SoPh..tmp..117B
  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.

---------------------------------------------------------
Title: Faraday Rotation Response to Coronal Mass Ejection Structure
Authors: Jensen, E. A.; Hick, P. P.; Bisi, M. M.; Jackson, B. V.;
   Clover, J.; Mulligan, T.
2010SoPh..265...31J    Altcode: 2010SoPh..tmp...75J
  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<SUB>1</SUB>, 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.

---------------------------------------------------------
Title: A Heliospheric Imager for Deep Space: Lessons Learned from
    Helios, SMEI, and STEREO
Authors: Jackson, B. V.; Buffington, A.; Hick, P. P.; Bisi, M. M.;
   Clover, J. M.
2010SoPh..265..257J    Altcode: 2010SoPh..tmp..102J
  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.

---------------------------------------------------------
Title: From the Sun to the Earth: The 13 May 2005 Coronal Mass
    Ejection
Authors: Bisi, M. M.; Breen, A. R.; Jackson, B. V.; Fallows, R. A.;
   Walsh, A. P.; Mikić, Z.; Riley, P.; Owen, C. J.; Gonzalez-Esparza,
   A.; Aguilar-Rodriguez, E.; Morgan, H.; Jensen, E. A.; Wood, A. G.;
   Owens, M. J.; 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.; Pintér, B.
2010SoPh..265...49B    Altcode: 2010SoPh..tmp..136B
  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.

---------------------------------------------------------
Title: Inclusion of In-Situ Velocity Measurements into the
    UCSD Time-Dependent Tomography to Constrain and Better-Forecast
    Remote-Sensing Observations
Authors: Jackson, B. V.; Hick, P. P.; Bisi, M. M.; Clover, J. M.;
   Buffington, A.
2010SoPh..265..245J    Altcode: 2010SoPh..tmp...43J; 2010SoPh..tmp...55J
  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.

---------------------------------------------------------
Title: The 13-15 May 2005 CME/ICME/MC: A Comprehensive Study from
    the Sun to the Earth
Authors: Bisi, Mario Mark; Breen, A. R.; Jackson, B. V.;
   Fallows, R. A.; Walsh, A. P.; Owens, M. J.; Riley, P.; Mikić,
   Z.; Gonzalez-Esparza, A.; Aguilar-Rodriguez, E.; Morgan, H.; Wood,
   A. G.; Jensen, E. A.; Tokumaru, M.; Manoharan, P. K.; Chashei, I. V.;
   Giunta, A. S.; Owen, C. J.; Fujiki, K.; Linker, J. A.; Shishov, V. I.;
   Tyul'bashev, S. A.; Agalya, G.; Glubokova, S. K.
2010shin.confE.126B    Altcode:
  Here, we present a brief overview of the results of a multi-technique,
  multi-instrument, co-ordinated study of the solar-eruptive and
  Earth-effective event(s) of 13-15 May 2005. We look at the resulting
  Earth-directed (halo) coronal mass ejection (CME), the interplanetary
  counterpart (ICME), and briefly, the flux-rope (Magnetic Cloud -
  MC) effects on the terrestrial space environment and upper Earth
  atmosphere. 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,
  as well as the use of coronal and heliospheric modelling. These analyses
  are subsequently used to trace the origin, development, propagation,
  terrestrial impact, and consequences of this event to obtain the
  most-comprehensive view (to our knowledge) of an Earth-effective solar
  eruption to date. Full details of the study of this event can be found
  in a comprehensive paper by Bisi et al., Solar Physics, Topical Issue
  (TI) on Remote Sensing of the Inner Heliosphere, 2010, when the TI is
  published in August/September 2010.

---------------------------------------------------------
Title: UCSD 3D Reconstruction of the 12 December 2008, 20 January
    2009, and 3 April 2010 CMEs
Authors: Clover, John M.; Jackson, B. V.; Hick, P. Paul; Buffington,
   A.; Amirbekian, N.
2010shin.confE.142C    Altcode:
  The Solar Mass Ejection Imager (SMEI) data base is available for the
  three-dimensional (3-D) reconstruction of CME/ICMEs from early 2003 up
  through the present. Here we concentrate upon analyses of three events,
  on 12 December 2008, 20 January 2009, and 3 April 2010; and provide
  comparisons with in-situ measurements during this interval. The
  University of California, San Diego (UCSD) SMEI database includes
  individual full-sky maps and orbit differences that preserve the
  original instrument resolution and photometric precision. Higher-level
  products (3-D reconstructions from the data, and 3-D tomographic
  reconstructed images are also maintained by UCSD on its SMEI website
  for the entire SMEI period of operation. The SMEI 3-D reconstruction
  program is now also available for use at the Community Coordinated
  Modeling Center (CCMC) located at the NASA/Goddard Space Flight Center.

---------------------------------------------------------
Title: UCSD IPS 3-D time-dependent reconstruction of the global
    solar wind during the last solar minimum
Authors: Jackson, Bernard V.; Clover, J. M.; Hick, P. Paul; Buffington,
   A.; Amirbekian, Narek
2010shin.confE.157J    Altcode:
  The University of California, San Diego (UCSD) maintains an
  interplanetary scintillation (IPS) data base from the Solar-Terrestrial
  Environment Laboratory (STELab), Nagoya, Japan, from the mid-1990's up
  to the present. UCSD's three-dimensional (3-D) reconstruction of these
  data in time-dependent format is available to provide measurements
  of global solar wind velocity and density for this entire period
  with a time cadence of one day when data from STELab are available
  (generally from April to December each year). Here we concentrate on
  analyses of measurements obtained during the recent solar minimum, and
  show time-dependent global solar wind velocity and density in several
  coordinate formats (e.g., Sun-centered ecliptic and heliographic,
  and as averaged per Carrington rotation). Velocity and density from
  these reconstructions are combined to also provide global solar wind
  dynamic pressure in these same formats. These analyses are used to
  determine the global extent and change of the solar wind during the
  last solar minimum. The current UCSD IPS 3-D reconstruction program
  is now also available for use at the Goddard Spaceflight Community
  Coordinated Modeling Center (CCMC) for analyses of specific time
  intervals and ICMEs.

---------------------------------------------------------
Title: Three-dimensional Reconstructions and Mass Determination of the
    2008 June 2 LASCO Coronal Mass Ejection Using STELab Interplanetary
    Scintillation Observations
Authors: Bisi, M. M.; Jackson, B. V.; Hick, P. P.; Buffington, A.;
   Clover, J. M.; Tokumaru, M.; Fujiki, K.
2010ApJ...715L.104B    Altcode:
  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<SUP>-1</SUP>. 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.

---------------------------------------------------------
Title: Solar Wind and CME Studies of the Inner Heliosphere Using
    IPS Data from Stelab, ORT, and EISCAT
Authors: 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.
2010aogs...21...33B    Altcode:
  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.

---------------------------------------------------------
Title: Solar Mass Ejection Imager (smei) and Interplanetary
    Scintillation (ips) 3D-RECONSTRUCTIONS of the Inner Heliosphere
Authors: Jackson, B. V.; Hick, P. P.; Buffington, A.; Bisi, M. M.;
   Clover, J. M.; Tokumaru, M.
2010aogs...21..339J    Altcode:
  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.

---------------------------------------------------------
Title: Solar Wind Speed Inferred from Cometary Plasma Tails using
    Observations from STEREO HI-1
Authors: Clover, John M.; Jackson, Bernard V.; Buffington, Andrew;
   Hick, P. Paul; Bisi, Mario M.
2010ApJ...713..394C    Altcode:
  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.

---------------------------------------------------------
Title: 3D Reconstruction of Density Enhancements Behind Interplanetary
    Shocks from Solar Mass Ejection Imager White-Light Observations
Authors: Jackson, B. V.; Hick, P. P.; Buffington, A.; Bisi, M. M.;
   Clover, J. M.; Hamilton, M. S.; Tokumaru, M.; Fujiki, K.
2010AIPC.1216..659J    Altcode:
  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.

---------------------------------------------------------
Title: Large-Scale Heliospheric Structure during Solar-Minimum
    Conditions using a 3D Time-Dependent Reconstruction Solar-Wind Model
    and STELab IPS Observations
Authors: Bisi, M. M.; Jackson, B. V.; Hick, P. P.; Clover, J. M.;
   Hamilton, S.; Tokumaru, M.; Fujiki, K.
2010AIPC.1216..355B    Altcode:
  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).

---------------------------------------------------------
Title: Solar Mass Ejection Imager (SMEI) near real time images and
    3-D reconstruction comparisons with multi-spacecraft observations
    during the rising phase of Solar Cycle 24
Authors: Jackson, Bernard; Clover, John; Hick, P.; Buffington, Andrew;
   Bisi, Mario
2010cosp...38.1873J    Altcode: 2010cosp.meet.1873J
  The Solar Mass Ejection Imager (SMEI) has been operating since February
  2003. At the University of California, San Diego (UCSD) we are now able
  to provide photometric images from SMEI in near real time. These are
  available in quick-look form as orbit-to-orbit difference sky maps in a
  variety of formats. A series of editing steps and a tomography program
  cleans these data sets of aurora and provides three-dimensional (3-D)
  volumetric density soon after the images become available, and allows us
  to map the 3-D density extents of interplanetary coronal mass ejections
  (ICMEs) and co-rotating structures. Here, we report on observations and
  3-D reconstructions from SMEI during the current rising phase of Solar
  Cycle 24. We match our analyses with in-situ densities from spacecraft
  near Earth as well as at the two STEREO spacecraft. These include
  both direct in-situ density variation comparisons and measurements of
  columnar mass fluxes for different events. These comparisons show the
  continuity of the structures that match in-situ density measurements
  at each spacecraft, and their extensions beyond the ecliptic plane.

---------------------------------------------------------
Title: Changes in gegenschein brightness with time, recorded by the
    solar mass ejection imager (SMEI)
Authors: Buffington, Andrew; Jackson, Bernard; Hick, P.; Clover, John
2010cosp...38..708B    Altcode: 2010cosp.meet..708B
  The Solar Mass Ejection Imager (SMEI), operating since February 2003,
  has provided photometric-quality visible-light maps covering nearly
  the entire sky, at a rate of roughly 15 per day for more than seven
  years. To measure the Gegenschein and characterize other aspects of
  the zodiacal light, we combine these maps into daily averages after
  subtracting individual bright stars, a residual sidereal background,
  and finally an empirical zodiacal-light model. From averages of
  the yearly brightness over the seven-year period, we find that the
  Gegenschein brightness has been steadily decreasing by about 2 percent
  per year. To confirm that this observation does not result from an error
  in assessing the change in imager response over this time, we also
  search for a potential brightness change of three comparably-bright
  but presumably unchanging sidereal objects, the Andromeda Galaxy and
  the two Magellanic Clouds. We find the brightness of these remains
  constant over this seven-year time period to better than 1 percent.

---------------------------------------------------------
Title: Measurements of the Gegenschein brightness from the Solar
    Mass Ejection Imager (SMEI)
Authors: Buffington, Andrew; Bisi, Mario M.; Clover, John M.; Hick,
   P. Paul; Jackson, Bernard V.; Kuchar, Thomas A.; Price, Stephan D.
2009Icar..203..124B    Altcode:
  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.

---------------------------------------------------------
Title: The Large-Scale Structure of the Solar Wind during Solar
    Minimum Conditions Using Three-Dimensional Reconstructions of
    Interplanetary Scintillation Data
Authors: Bisi, Mario Mark; Jackson, Bernard V.; Clover, John M.;
   Tokumaru, Munetoshi; Fujiki, Ken'ichi; Breen, Andrew R.; Fallows,
   Richard A.; Buffington, Andrew; Hick, P. Paul
2009shin.confE.149B    Altcode:
  Interplanetary scintillation (IPS) observations provide information
  about a large portion of the inner heliosphere. We use Solar-Terrestrial
  Environment Laboratory (STELab) IPS velocity and g-level observations as
  well as IPS velocity observations from the European Incoherent SCATter
  (EISCAT) and EISCAT Svalbard Radar (ESR), with our three-dimensional
  (3D) reconstruction data processing to determine velocities and
  densities of the inner heliosphere. Here, we concentrate primarily on
  results covering the 2007-2009 International Heliophysical Year (IHY)
  which includes the Whole Heliosphere Interval (CR2068). We present
  these using various forms of imaging from our time-dependent modelled
  calculations that can measure changes with durations of less than a day,
  and compare these with various spacecraft in-situ measurements. We
  also present synoptic maps from the reconstructions. These maps
  show large-scale solar wind structure during the somewhat unusual
  solar-minimum conditions, in relation to transients that are present
  during this period. These maps are also available as differences
  relative to a Carrington-averaged background.

---------------------------------------------------------
Title: Measurements of White-Light Images of Comet Plasma Tails as
    a Proxy for Solar Wind Speed
Authors: Clover, John M.; Bisi, Mario M.; Buffington, Andrew; Jackson,
   Bernard V.; Hick, P. Paul
2009shin.confE..51C    Altcode:
  The high temporal and spatial resolution of heliospheric white-light
  imagers enables us to measure the changes in plasma tails of bright
  comets. Plasma tails of comets have been recognized as natural
  probes of the solar wind for many years, and thus using the technique
  developed at the University of California, San Diego to measure the
  changes in the plasma tails of comets, we obtain measurements for
  the speed of the solar wind in situ. We present the results of this
  technique used successfully on multiple comets observed by the Solar
  Mass Ejection Imager (SMEI) and Heliospheric Imagers on board the
  twin Solar TErrestrial RElations Observatory (STEREO) spacecraft,
  and discuss future applications.

---------------------------------------------------------
Title: The UCSD Solar Mass Ejection Imager (SMEI) and Interplanetary
    Scintillation (IPS) 3D Reconstruction Analyses and Databases now at
    the CCMC
Authors: Jackson, Bernard V.; Bisi, Mario M.; Clover, John M.; Hick,
   P. Paul; Buffington, Andrew
2009shin.confE..42J    Altcode:
  Both the Solar Mass Ejection Imager (SMEI) and interplanetary
  scintillation (IPS) data bases and 3D modeling are now available and
  operate at the Community Coordinated Modeling Center (CCMC). We present
  the current state of these instrument's databases that are maintained
  and stored on UCSD/CASS Web servers. The IPS database is available for
  real-time access from the Solar-Terrestrial Environment Laboratory
  (STELab), Japan, and the UCSD IPS Web site provides a variety of
  higher-level data products derived from these observations to help
  in Space Weather Forecasting. The up-to-date UCSD SMEI database
  includes individual SMEI CCD data frames from each of the three SMEI
  cameras since first light in February 2003, as well as full-sky maps
  in a sidereal reference frame that preserve the original instrument
  resolution and photometric precision. Higher-level products from this
  database and 3-D tomographic reconstruction images are also maintained
  by UCSD on its SMEI website for the entire SMEI operation interval.

---------------------------------------------------------
Title: Fabrication and test of a diamond-turned mirror suitable for
    a spaceborne photometric heliospheric imager
Authors: Buffington, Andrew; Bach, Kirk G.; Bach, Bernhard W.; Bach,
   Erich K.; Bisi, Mario M.; Hick, P. Paul; Jackson, Bernard V.; Klupar,
   Peter D.
2009SPIE.7438E..0OB    Altcode: 2009SPIE.7438E..17B
  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.

---------------------------------------------------------
Title: Studying geoeffective interplanetary coronal mass ejections
between the Sun and Earth: Space weather implications of Solar Mass
    Ejection Imager observations
Authors: Webb, D. F.; Howard, T. A.; Fry, C. D.; Kuchar, T. A.;
   Mizuno, D. R.; Johnston, J. C.; Jackson, B. V.
2009SpWea...7.5002W    Altcode: 2009SpWea...705002W
  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.

---------------------------------------------------------
Title: Study of CME Propagation in the Inner Heliosphere: SOHO LASCO,
    SMEI and STEREO HI Observations of the January 2007 Events
Authors: 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.
2009SoPh..256..239W    Altcode:
  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 (&gt; 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.

---------------------------------------------------------
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
Authors: Bisi, M. M.; Jackson, B. V.; Buffington, A.; Clover, J. M.;
   Hick, P. P.; Tokumaru, M.
2009SoPh..256..201B    Altcode:
  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.

---------------------------------------------------------
Title: Three-Dimensional Reconstructions of the Solar Wind: During
    Solar Minimum Conditions
Authors: Bisi, Mario; Jackson, B. V.; Hick, P. P. L.; Clover, J. M.;
   Tokumaru, M.; Fujiki, K.; Fallows, R. A.; Breen, A. R.
2009SPD....40.3203B    Altcode:
  Interplanetary scintillation (IPS) observations provide information
  about a vast region of the inner heliosphere. We use Solar-Terrestrial
  Environment Laboratory (STELab) IPS velocity and g-level observations as
  well as IPS velocity observations from the European Incoherent SCATter
  (EISCAT) and EISCAT Svalbard Radar (ESR), with our three-dimensional
  (3D) reconstruction model to determine velocities and densities of the
  inner heliosphere. We present these observations using various forms
  of imaging from our time-dependent model that can measure changes with
  durations of less than a day and compare these with various spacecraft
  in situ measurements. We concentrate on the current solar-minimum period
  showing relatively-stable large-scale solar-wind structure during this
  time in relation to transients that are also sometimes present. Data
  primarily covers the 2007-2009 International Heliophysical Year (IHY)
  which includes the Whole Heliosphere Interval (CR2068).

---------------------------------------------------------
Title: CMEs In The Heliosphere Observed With Combined Imaging And
    In-situ Data From LASCO, Stereo And SMEI
Authors: Webb, David F.; Biesecker, D.; Howard, T. A.; Luhmann, J. G.;
   Li, Y.; Galvin, A.; Howard, R. A.; Jackson, B. V.
2009SPD....40.2102W    Altcode:
  Despite being in solar activity minimum, there have been a number
  of events in which a CME observed at the Sun by one or both STEREO
  spacecraft has passed over one of them (or the Earth) as detected from
  in-situ data. These form a special class of space weather-type events
  that can provide information on the characteristics of the geometry,
  propagation and internal structure of CMEs. Important to this study are
  the remote imaging observations from the SECCHI Heliospheric Imagers
  (HIs) and, occasionally, also from the Solar Mass Ejection Imager
  (SMEI) in Earth orbit. HI and SMEI observations of ICMEs can provide
  complementary information. I will review these types of events and
  summarize their characteristics and what they tell us about CMEs.

---------------------------------------------------------
Title: 3D-Reconstruction of Density Enhancements Behind Interplanetary
    Shocks from Solar Mass Ejection White-Light Observations
Authors: Jackson, Bernard V.; Hick, P. P. L.; Buffington, A.; Bisi,
   M. M.; Clover, J. M.; Tokumaru, M.; Fujiki, K.
2009SPD....40.2101J    Altcode:
  The Solar Mass Ejection Imager (SMEI) observes the increased brightness
  from the density enhancements behind interplanetary shocks that are
  observed in situ near the Earth. We use the University of California,
  San Diego time-dependent three-dimensional-reconstruction technique
  to map the extents of these density enhancements. As examples,
  we examine the shock density enhancements associated with several
  well-known coronal mass ejections including the 28 October 2003
  (Halloween storm) event. We compare these density enhancements with
  reconstructed velocity observations from Solar-Terrestrial Environment
  Laboratory interplanetary scintillation (IPS) observations when these
  are available. Volumetric-differencing techniques available from the
  SMEI analyses show that the outer portion of a larger increase in
  heliospheric density is often what is observed in short-time image
  brightness subtractions from these data.

---------------------------------------------------------
Title: Coronal Mass Ejection Reconstructions from Interplanetary
Scintillation Data Using a Kinematic Model: A Brief Review
Authors: Bisi, M. M.; Jackson, B. V.; Hick, P. P.; Buffington, A.;
   Clover, J. M.
2009aogs...14..161B    Altcode:
  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° latitudinal and longitudinal
  heliographic resolution for a co-rotational model, and a one-day
  cadence and 20° 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.

---------------------------------------------------------
Title: Solar Wind 3D Reconstructions of the Whole Heliospheric
    Interval
Authors: Bisi, M. M.; Jackson, B. V.; Clover, J. M.; Hick, P. P.;
   Buffington, A.; Manoharan, P. K.; Tokumaru, M.
2008AGUFMSH23A1617B    Altcode:
  3D tomographic reconstructions of the inner heliosphere have been used
  for over a decade to visualise and investigate the structure of the
  solar wind and its various features such as transients and corotating
  structures. Interplanetary scintillation (IPS) observations of the
  solar wind have been carried out for a much longer period of time
  revealing information on the structure of the solar wind and the
  features within it. Here we present such 3D reconstructions using
  IPS observations from the Solar Terrestrial Environment Laboratory
  (STELab) and the Ootacamund (Ooty) Radio Telescope (ORT) of the Whole
  Heliospheric Interval (WHI) Carrington Rotation 2068. This is part of
  the world-wide IPS community's International Heliosphysical Year (IHY)
  collaboration. We show the structure of the inner heliosphere during
  this time and how our global reconstructions compare with deep-space
  spacecraft measurements such as those taken by Wind, ACE, STEREO,
  and Ulysses in terms of density and velocity.

---------------------------------------------------------
Title: SMEI Remote Sensing and the 3D Reconstruction of Corotating
    Heliospheric Structures
Authors: Jackson, B. V.; Bisi, M. M.; Hick, P. P.; Buffington, A.;
   Clover, J. M.; Webb, D. F.; Tokumaru, M.; Manoharan, P. K.
2008AGUFMSH13B1554J    Altcode:
  We report observations and 3D reconstructions of corotating
  heliospheric structures observed by the Solar Mass Ejection Imager
  (SMEI). Observations of the inner heliosphere have been carried out
  on a routine basis by SMEI since its launch in early 2003, and these
  have been used to measure and map the outward flow of several-hundred
  CMEs. Most of these observations use short-term variations of
  brightness from one SMEI orbit to the next (every 102 minutes)
  to track outward motion. The disadvantage of these orbit-to-orbit
  analyses is that they cannot measure features that remain stationary
  relative to the Sun-Earth line (or those which corotate with the Sun)
  and change slowly over time periods of several days. At UCSD we provide
  measurements of heliospheric structures relative to a long-term base
  and, even in these observations, there is little evidence of long-term
  stationary-standing density structures that corotate. By employing a
  kinematic model of the solar wind, we reconstruct three-dimensional
  (3D) solar wind structures from multiple observing lines of sight
  through the outward-flowing solar wind. By including interplanetary
  scintillation (IPS) velocity observations from STELab, Japan or from
  Ooty, India we can extract both the solar wind density and velocity
  from these analyses to compare with "ground truth" measurements from
  multi-point, in-situ solar wind measurements from the STEREO, SOHO,
  Wind, and ACE spacecraft. We define the heliospheric structures by
  these 3D velocity analyses, and they show that while the velocities
  map large regions near the ecliptic that corotate, the dense structures
  that front and follow these regions are far more tenuous.

---------------------------------------------------------
Title: Modeling the Corona-Heliosphere Interface in Anticipation of
    the Murchison Wide-field Array
Authors: Kasper, J. C.; Oberoi, D.; Salah, J. E.; Jackson, B. V.;
   Cairns, I.
2008AGUFMSH11A..03K    Altcode:
  The Murchison Widefield Array (MWA) is an 8,000-antenna, 80-300 MHz,
  imaging radio array under construction in Western Australia that
  features a large field of view, high sensitivity, and accurate
  polarization and intensity calibration. An MWA prototype has
  been deployed in the field and construction of the full array
  will begin in mid-2009 after the performance of the prototype is
  evaluated. Understanding the connection between the upper corona and
  the inner heliosphere with novel low-frequency radio observations is
  a primary objective of the MWA Solar, Heliospheric, and Ionospheric
  (SHI) science consortium. This presentation covers progress by the
  SHI consortium's theory and modeling effort. We show simulations of
  how Faraday rotation, interplanetary scintillation, and radio burst
  measurements can track and constrain the transport of magnetic fields,
  density, and energetic electrons into the heliosphere.

---------------------------------------------------------
Title: Observation and Modeling of Ion Upwelling Above Aurora
Authors: Lummerzheim, D.; Otto, A.; Doe, R. A.; Jackson, B. V.;
   Mizuno, D.; Webb, D. F.; Collins, R. L.; Light, A. S.
2008AGUFMSA21B1542L    Altcode:
  Auroral electron precipition heats the ionospheric plasma. Especially
  at F-region altitudes, this leads to increased plasma pressure and a
  pressure gradient force that accelerates plasma away from the heated
  region. The resulting upward ion velocities have been observed by the
  incoherent scatter radar at Poker Flat (PFISR). The upward moving
  ions cause an increased ion density well above typical auroral
  ionization altitudes. N2+ ions that are lifted to altitudes above
  the shadowheight will resonantly scatter sunlight. This is observed
  by coincident overflights of the Solar Mass Ejection Imager (SMEI)
  on the Coriolis satellite, looking up from 840 km altitude. We will
  present a study that combines modeling and observations by PFISR and
  SMEI to illustrate and explain this process.

---------------------------------------------------------
Title: Measurements of the Gegenschein brightness from the Solar
    Mass Ejection Imager (SMEI)
Authors: Buffington, A.; Bisi, M. M.; Clover, J. M.; Hick, P.; Jackson,
   B. V.
2008AGUFMSH13B1561B    Altcode:
  The Gegenschein is a faint diffuse component of the zodiacal light
  centered upon the antisolar point; this has now been viewed by the
  Solar Mass Ejection Imager (SMEI) for over 5 years. SMEI provides
  unprecedented near-full-sky photometric maps each 102-minute orbit,
  using data from 3 unfiltered CCD cameras. Its 0.1% photometric precision
  enables observation over long periods of time, of heliospheric
  structures having surface brightness down to several S10's (an S10
  is the equivalent brightness of a 10th magnitude star spread over
  one square degree). When individual bright stars are removed from the
  maps and an empirical sidereal background subtracted, the residue is
  dominated by the zodiacal light. The sky coverage and duration of these
  measurements enables a definitive characterization. We describe the
  analysis method for these data, characterize the average Gegenschein
  brightness distribution, present empirical formulae describing its
  shape, and discuss its variation with time.

---------------------------------------------------------
Title: The Solar Eruption of 2005 May 13 and Its Effects:
    Long-Baseline Interplanetary Scintillation Observations of the
    Earth-Directed Coronal Mass Ejection
Authors: Breen, A. R.; Fallows, R. A.; Bisi, M. M.; Jones, R. A.;
   Jackson, B. V.; Kojima, M.; Dorrian, G. D.; Middleton, H. R.;
   Thomasson, P.; Wannberg, G.
2008ApJ...683L..79B    Altcode:
  Long-baseline observations of interplanetary scintillation (IPS)
  provide a unique source of information on solar wind speed and
  meridional direction across the inner regions of the solar system. We
  report the results of a series of coordinated IPS observations of an
  Earth-directed CME. A significant development in the interpretation of
  these data is the use of 3D tomographic reconstructions of solar wind
  structure derived from STELab IPS data to better constrain the analysis
  of extremely long baseline observations from EISCAT and MERLIN. The
  combination of these two approaches leads to a significantly better
  understanding of the interaction of the CME with the background
  solar wind than would be possible with either technique alone,
  revealing a significant rotation in the meridional flow direction of
  the background wind associated with the passage of the CME. The CME
  itself is decelerated significantly between its emergence through the
  corona and its arrival in the IPS ray path, with comparatively little
  change in speed from then until arrival at ACE.

---------------------------------------------------------
Title: SMEI Observations of the Heliosphere During WHI
Authors: Jackson, B. V.; Bisi, M. M.; Hick, P. P.; Buffington, A.;
   Clover, J. M.; Webb, D. F.
2008AGUSMSH51A..08J    Altcode:
  Solar Mass Ejection Imager (SMEI) observations of the inner heliosphere
  have been carried out on a routine basis since early 2003. By employing
  a kinematic model of the solar wind, we reconstruct three-dimensional
  (3D) solar wind structures from multiple observing lines of sight
  through the outward-flowing solar wind. These models allow us to extract
  solar wind density and to compare these to "ground truth" measurements
  from multi- point in-situ solar wind measurements from the STEREO,
  SOHO, ACE, and the Wind spacecraft. This aids in improving the 3D
  reconstruction technique by comparing these reconstructions at multiple
  points in the inner heliosphere. Because our observations reveal the
  global nature of heliospheric structures, this also leads to a better
  understanding of the structure and dynamics of the interplanetary
  environment around each spacecraft, and how these structures are
  connected back to the Sun. During the Whole Heliosphere Interval (WHI)
  SMEI will provide views and 3D reconstructions of the global heliosphere
  that can be compared with ground-based and spacecraft observations.

---------------------------------------------------------
Title: Numerical Simulations of Solar Wind Disturbances by Coupled
    Models
Authors: Odstrcil, D.; Pizzo, V. J.; Arge, C. N.; Bissi, M. M.; Hick,
   P. P.; Jackson, B. V.; Ledvina, S. A.; Luhmann, J. G.; Linker, J. A.;
   Mikic, Z.; Riley, P.
2008ASPC..385..167O    Altcode:
  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.

---------------------------------------------------------
Title: Observations of a comet tail disruption induced by the passage
    of a CME
Authors: 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.
2008JGRA..113.4101K    Altcode: 2008JGRA..11304101K
  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.

---------------------------------------------------------
Title: Analysis of Plasma-Tail Motions for Comets C/2001 Q4 (NEAT)
    and C/2002 T7 (LINEAR) Using Observations from SMEI
Authors: Buffington, A.; Bisi, M. M.; Clover, J. M.; Hick, P. P.;
   Jackson, B. V.; Kuchar, T. A.
2008ApJ...677..798B    Altcode:
  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, lesssim0.05 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<SUP>-1</SUP> lower than before or afterward. Time durations of
  such events vary, typically from 3 to 8 hr, and correspond to comet
  traversal distances ~10<SUP>6</SUP> 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.

---------------------------------------------------------
Title: Solar Mass Ejection Imager 3-D reconstruction of the 27-28
    May 2003 coronal mass ejection sequence
Authors: Jackson, B. V.; Bisi, M. M.; Hick, P. P.; Buffington, A.;
   Clover, J. M.; Sun, W.
2008JGRA..113.0A15J    Altcode:
  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.

---------------------------------------------------------
Title: Three-dimensional reconstructions of the early November 2004
Coordinated Data Analysis Workshop geomagnetic storms: Analyses of
    STELab IPS speed and SMEI density data
Authors: Bisi, M. M.; Jackson, B. V.; Hick, P. P.; Buffington, A.;
   Odstrcil, D.; Clover, J. M.
2008JGRA..113.0A11B    Altcode:
  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.

---------------------------------------------------------
Title: Comparison of the extent and mass of CME events in the
    interplanetary medium using IPS and SMEI Thomson scattering
    observations
Authors: Jackson, B. V.; Hick, P. P.; Buffington, A.; Bisi, M. M.;
   Kojima, M.; Tokumaru, M.
2007A&AT...26..477J    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: IPS tomographic observations of 3D solar wind structure
Authors: Kojima, M.; Tokumaru, M.; Fujiki, K.; Hayashi, K.; Jackson,
   B. V.
2007A&AT...26..467K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: IPS observations of the inner-heliosphere and their comparison
    with multi-point in-situ measurements
Authors: Bisi, M. M.; Jackson, B. V.; Breen, A. R.; Fallows, R. A.;
   Feynman, J.; Clover, J. M.; Hick, P. P.; Buffington, A.
2007AGUFMSH33A1091B    Altcode:
  Interplanetary scintillation (IPS) observations of the inner-heliosphere
  have been carried out on a routine basis for many years using
  metre-wavelength radio telescope arrays. By employing a kinematic
  model of the solar wind, we reconstruct the three-dimensional (3D)
  structure of the inner-heliosphere from multiple observing lines of
  sight. From these reconstructions we extract solar wind parameters
  such as velocity and density, and compare these to "ground truth"
  measurements from multi-point in situ solar wind measurements from
  ACE, Ulysses, STEREO, and the Wind spacecraft, particularly during
  the International Heliophysical Year (IHY). These multi- point
  comparisons help us improve our 3D reconstruction technique. Because
  our observations show heliospheric structures globally, this leads to a
  better understanding of the structure and dynamics of the interplanetary
  environment around these spacecraft.

---------------------------------------------------------
Title: Analysis and Interpretation of Comet Measurements from SMEI
Authors: Buffington, A.; Bisi, M. M.; Clover, J. M.; Hick, P. P.;
   Jackson, B. V.
2007AGUFMSH33A1080B    Altcode:
  The Solar Mass Ejection Imager (SMEI) has observed several comets and
  traced their plasma tails as far as 108 km from their nucleus. A time
  sequence of SMEI orbital sky maps displays considerable tail motion and
  disruption for several of these comets. Tracking these motions versus
  time, when combined with ephemeris information about their distance
  from the Earth allows a determination of solar wind speeds and their
  variation with the location of the comet. In the case of comets C/2001
  Q4 (NEAT) and C/2002 T7 (LINEAR), which passed within about 0.3 AU of
  Earth in April and May of 2004, the SMEI observations show that speeds
  during disruptions are typically 50 to 100 km s-1 less than speeds
  before and after. Time durations of the disturbances vary between 3
  and 8 hours, and correspond to distances traversed by the comets of
  ~106 km (0.007 AU). We compare these observations with interplanetary
  scintillation (IPS) three-dimensional tomographic reconstructions and
  find no evidence that the comet-tail features are due to large-scale
  density or velocity structures. We also compare these with near-by
  spacecraft measurements such as the Advanced Composition Explorer
  (ACE), and find a similar result. This suggests that the comet-tail
  disruptions are caused by small-scale changes in the solar wind acting
  over distances that are short compared with 1 AU.

---------------------------------------------------------
Title: Inner-heliosphere SMEI observations and their comparison with
    multi-point in-situ measurements
Authors: Jackson, B. V.; Bisi, M. M.; Hick, P. P.; Buffington, A.;
   Clover, J. M.; Feynman, J.
2007AGUFMSH51B..03J    Altcode:
  Solar Mass Ejection Imager (SMEI) observations of the inner heliosphere
  have been carried out on a routine basis since shortly after its launch
  on January 6, 2003. By employing a kinematic model of the solar wind,
  we reconstruct three-dimensional (3D) solar wind structures from
  multiple observing lines of sight through the outward-flowing solar
  wind. This model allows us to extract solar wind densities from the
  SMEI white-light observations and to compare these to multi-point in
  situ "ground truth" solar wind measurements from instruments aboard
  the Ulysses, STEREO, ACE, and Wind spacecraft. This facilitates
  improvements to our 3D reconstruction technique by comparing these
  reconstructions at multiple points in the inner-heliosphere. Our
  observations show heliospheric structures globally, and because of
  this, our reconstructions provide us with a better understanding of
  the structure and dynamics of the interplanetary environment around
  each spacecraft, and how these structures are connected back to the Sun.

---------------------------------------------------------
Title: How Does Large Flaring Activity from the Same Active Region
    Produce Oppositely Directed Magnetic Clouds?
Authors: Harra, Louise K.; Crooker, Nancy U.; Mandrini, Cristina H.;
   van Driel-Gesztelyi, Lidia; Dasso, Sergio; Wang, Jingxiu; Elliott,
   Heather; Attrill, Gemma; Jackson, Bernard V.; Bisi, Mario M.
2007SoPh..244...95H    Altcode:
  We describe the interplanetary coronal mass ejections (ICMEs) that
  occurred as a result of a series of solar flares and eruptions from
  4 to 8 November 2004. Two ICMEs/magnetic clouds occurring from these
  events had opposite magnetic orientations. This was despite the fact
  that the major flares related to these events occurred within the same
  active region that maintained the same magnetic configuration. The solar
  events include a wide array of activities: flares, trans-equatorial
  coronal loop disappearance and reformation, trans-equatorial filament
  eruption, and coronal hole interaction. The first major ICME/magnetic
  cloud was predominantly related to the active region 10696 eruption. The
  second major ICME/magnetic cloud was found to be consistent with the
  magnetic orientation of an erupting trans-equatorial filament or else
  a rotation of 160° of a flux rope in the active region. We discuss
  these possibilities and emphasize the importance of understanding the
  magnetic evolution of the solar source region before we can begin to
  predict geoeffective events with any accuracy.

---------------------------------------------------------
Title: CME 3D Reconstructions Using Solar Mass Ejection Imager and
    Interplanetary Scintillation Data
Authors: Jackson, Bernard V.; Bisi, M. M.; Hick, P. P.; Buffington, A.
2007AAS...210.2923J    Altcode: 2007BAAS...39..141J
  Solar Mass Ejection Imager (SMEI) and interplanetary scintillation (IPS)
  observations provide a view of the solar wind at all solar elongations;
  from 180 degrees anti-solar to as close to the Sun as coronagraph
  fields of view. They can be used to study the evolution of the solar
  wind and solar transients out into interplanetary space. In addition,
  the inner heliospheric response to corotating solar structures and
  coronal mass ejections (CMEs) can be measured, both in scintillation
  level and in velocity when using IPS, and through Thomson Scattering
  when using SMEI. We use a 3D reconstruction technique that obtains
  perspective views from solar corotating plasma and outward-flowing
  solar wind as observed from Earth, by iteratively fitting a kinematic
  solar wind model to both SMEI and IPS observations. This 3D modeling
  technique permits reconstructions of the density and velocity structures
  of CMEs and other interplanetary transients. These reconstructions
  have a temporal cadence and heliographic latitudinal and longitudinal
  resolution predicated by the amount of data used for time-dependent
  reconstructions, and can use data from a variety of IPS instruments
  distributed around the Earth. We highlight the 3D analyses of these
  different data sets using a series of CME events observed beginning on
  the Sun 4-7 November 2004. We also apply this technique to determine
  solar wind pressure (“ram” pressure) at Mars. Results are compared
  with ram pressure observations derived from Mars Global Surveyor
  magnetometer data for the years 1999 through 2004, and include a
  reconstruction of a “back-side” event as seen by SOHO/LASCO.

---------------------------------------------------------
Title: The source and propagation of the interplanetary disturbance
    associated with the full-halo coronal mass ejection on 28 October 2003
Authors: Tokumaru, Munetoshi; Kojima, Masayoshi; Fujiki, Ken'Ichi;
   Yamashita, Masahiro; Jackson, Bernard V.
2007JGRA..112.5106T    Altcode: 2007JGRA..11205106T
  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.

---------------------------------------------------------
Title: Analysis of Solar Wind Events Using Interplanetary
    Scintillation Remote Sensing 3D Reconstructions and Their Comparison
    at Mars
Authors: Jackson, B. V.; Boyer, J. A.; Hick, P. P.; Buffington, A.;
   Bisi, M. M.; Crider, D. H.
2007SoPh..241..385J    Altcode:
  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° latitudinal and longitudinal resolution for the corotational
  model and a one-day cadence and 20° 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° west
  of the Sun - Earth line by the Mars Global Surveyor with the response
  derived from the IPS 3D reconstructions.

---------------------------------------------------------
Title: 3-D Magnetic Field Geometry of the October 28, 2003 ICME:
    Comparison with SMEI White-Light Observations
Authors: Jensen, E. A.; Mulligan, T.; Jackson, B. V.; Tokumaru, M.
2006AGUFMSH33A0397J    Altcode:
  Multiple reconstructions of the October 28-29, 2003 CME/ICME using
  white-light observations, ground-based cosmic-ray and in situ magnetic
  field flux rope modeling show two possible flux-rope configurations
  that pass Earth on opposite sides of the central symmetry axis of the
  disturbance. An analysis of flux rope model geometries initiated over
  a wide range in parameter space to test the uniqueness of the single
  spacecraft inversion reveals the fit is degenerate over a range of
  impact parameters such that two solutions are obtained. In one case (fit
  A) the disturbance passes Earth to the west of the rope center with the
  rope axis at a low inclination of 20 deg to the ecliptic, similar to
  the ground-based flux rope analysis by Kuwabara et al.~(2004). In the
  second case (fit B) the disturbance passes Earth to the east of the flux
  rope axis, with the rope axis more highly inclined at 42 deg from the
  ecliptic, consistent with the SMEI white-light analysis of Jackson et
  al.~(2006). The current densities in both solutions indicate a nearly
  force-free structure. Multipoint studies of ICMEs show the radius of
  curvature in the plane of the rope is between that of a dipole field
  line connected to the Sun and that of a circular field line connected
  to the Sun. Assuming a dipole field geometry for the large- scale
  axial field curvature of the rope results in a 3-D reconstruction
  for case B that is consistent with the loop structure and observed
  speed in the white-light LASCO images and SMEI density reconstruction,
  but not for case A. Multipoint measurements of large-scale solar wind
  transients is one of the key objectives of the Stereo mission, allowing
  more accurate 3-D reconstructions of in situ data for comparison with
  white-light observations. Until they become available, the large-scale
  axial field orientation and loop geometry of these rope reconstructions
  provides another tool to constrain magnetic flux rope fits of ICMEs
  using single spacecraft measurements.

---------------------------------------------------------
Title: Solar Mass Ejection Imager (SMEI) observations of coronal
    mass ejections (CMEs) in the heliosphere
Authors: 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.
2006JGRA..11112101W    Altcode:
  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.

---------------------------------------------------------
Title: An Empirical Description of Zodiacal Light as Measured by SMEI
Authors: Buffington, A.; Jackson, B. V.; Hick, P.; Price, S. D.
2006AGUFMSH32A..06B    Altcode:
  The SMEI visible-light cameras provide a photometric skymap for each
  102-minute orbit with the objective to observe transient Coronal Mass
  Ejections (CMEs). Zodiacal light is a significant contributor to these
  maps and must be removed in the data-analysis in order to detect and
  characterize the much fainter CMEs. We have analyzed over three years
  of the SMEI calibration data that were taken at the highest spatial
  resolution to derive the yearly averaged global distribution of zodiacal
  light between solar elongations of 20 and 180 degrees. Residuals on
  the individual sky maps from this global average provide information
  on the detailed geometry of the clouds. We present preliminary results
  of the analysis, including a characterization of the Gegenschein,
  possible dust bands, and annual variations.

---------------------------------------------------------
Title: The 20 January 2005 CME Solar Mass Ejection Imager (SMEI)
    Analyses
Authors: Jackson, B. V.; Hick, P. P.; Buffington, A.
2006AGUFMSH33A0396J    Altcode:
  Solar Mass Ejection Imager (SMEI) brightness measurements are analyzed
  to determine 3D volumetric densities for several CMEs including
  that of the 20 January 2005 CME. Here we present analyses of these 3D
  heliospheric volumetric solar wind density analyses. We use this system
  to measure the distribution of structure and provide a 3D mass of the
  ejecta associated with the large CMEs viewed in SMEI observations. In
  the case of the 20 January 2005 CME, the primary mass moves to the
  northwest of the Sun following the event observed earlier in LASCO
  coronagraph observations. There are two other very large coronal
  responses to the coronal energy input beginning around 6:30 UT near
  the time of CME onset. One of these is the large and extremely prompt
  Solar Energetic Particle (SEP) proton event observed at Earth beginning
  about 6:50 UT. Another response is an outward-propagating fast shock
  that arrives at Earth 34 hours following the event onset. A response
  that may be attributed to this shock is observed slightly more than
  5 days following this at the Ulysses spacecraft situated 5.3 AU from
  the Sun, 17 degrees south of the ecliptic, and 27 degrees from the
  Sun-Earth line to the west. SMEI observes the white-light response of
  this shock at Earth in the interplanetary medium around the spacecraft,
  and limits the shock extent in 3D.

---------------------------------------------------------
Title: CME Brightness at Large Elongations: Application to LASCO
    and SMEI Observations
Authors: Vourlidas, A.; Webb, D. F.; Morrill, J. S.; Jackson, B. V.
2006AGUFMSH32A..03V    Altcode:
  The traditional analysis of the CME brightness relied on the assumption
  that all lines of sight through the CME were parallel due to the large
  distance between the observer and the event. However, this assumption
  is not correct when CME observations at large distances from the
  Sun are concerned. In a recent paper (Vourlidas &amp; Howard 2006)
  we have outlined the proper geometry and presented a few theoretical
  predictions about the brightness evolution of CME launched at various
  angles relative to the Sun-observer line. In this talk, we use LASCO
  and SMEI observations of the same events to test our predictions and
  see how we can use our theoretical framework to interpret the observed
  CME structures.

---------------------------------------------------------
Title: The Evolution of Comets in the Heliosphere as Observed by SMEI
Authors: Kuchar, T.; Buffington, A.; Howard, T.; Arge, C. N.; Webb,
   D.; Jackson, B. V.; Hick, P. P.
2006AGUFMSH32A..08K    Altcode:
  Comet observations have been used as in situ probes of the heliospheric
  environment since they were used to confirm the existence of the solar
  wind. Changes in a comet tail's appearance are attributed to changes
  in the solar wind flow. Large scale tail disruptions are usually
  associated with boundary crossings of the current sheet or, more
  rarely, impacts from coronal mass ejections. The Solar Mass Ejection
  Imager (SMEI) observed three bright comets during April-May 2004:
  Bradfield (C/2004 F4), LINEAR (C/2002 T7), and NEAT (C/2001 Q4). We
  had previously reported several comet tail disconnection events (DEs)
  for both NEAT and LINEAR. Investigation of the entire period further
  reveals that these two comets showed continual changes in their
  plasma tails. These changes are characterized by a "smokestack-like"
  billowing effect punctuated by the disconnections. Bradfield however
  was remarkably quiescent during this entire period. We present these
  extended comet observations and offer an analysis and cause of the
  similarities and disparities of these data.

---------------------------------------------------------
Title: International Colloquium "Scattering and Scintillation in
    Radio Astronomy" was held on June 19-23, 2006 in Pushchino, Moscow
    region, Russia
Authors: Shishov, V. I.; Coles, W. A.; Rickett, B. J.; Bird,
   M. K.; Efimov, A. I.; Samoznaev, L. N.; Rudash, V. K.; Chashei,
   I. V.; Plettemeier, D.; Spangler, S. R.; Tokarev, Yu.; Belov, Yu.;
   Boiko, G.; Komrakov, G.; Chau, J.; Harmon, J.; Sulzer, M.; Kojima,
   M.; Tokumaru, M.; Fujiki, K.; Janardhan, P.; Jackson, B. V.; Hick,
   P. P.; Buffington, A.; Olyak, M. R.; Fallows, R. A.; Nechaeva, M. B.;
   Gavrilenko, V. G.; Gorshenkov, Yu. N.; Alimov, V. A.; Molotov, I. E.;
   Pushkarev, A. B.; Shanks, R.; Tuccari, G.; Lotova, N. A.; Vladimirski,
   K. V.; Obridko, V. N.; Gubenko, V. N.; Andreev, V. E.; Stinebring, D.;
   Gwinn, C.; Lovell, J. E. J.; Jauncey, D. L.; Senkbeil, C.; Shabala, S.;
   Bignall, H. E.; Macquart, J. -P.; Rickett, B. J.; Kedziora-Chudczer,
   L.; Smirnova, T. V.; Rickett, B. J.; Malofeev, V. M.; Malov, O. I.;
   Tyulbashev, S. A.; Jessner, A.; Sieber, W.; Wielebinski, R.
2006astro.ph..9517S    Altcode:
  Topics of the Colloquium: a) Interplanetary scintillation b)
  Interstellar scintillation c) Modeling and physical origin of the
  interplanetary and the interstellar plasma turbulence d) Scintillation
  as a tool for investigation of radio sources e) Seeing through
  interplanetary and interstellar turbulent media Ppt-presentations are
  available on the Web-site: http://www.prao.ru/conf/Colloquium/main.html

---------------------------------------------------------
Title: Preliminary three-dimensional analysis of the heliospheric
    response to the 28 October 2003 CME using SMEI white-light
    observations
Authors: Jackson, B. V.; Buffington, A.; Hick, P. P.; Wang, X.;
   Webb, D.
2006JGRA..111.4S91J    Altcode: 2006JGRA..11104S91J
  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° elongation
  (angular distance) from the solar disk until it fades in the antisolar
  hemisphere in the SMEI 180° 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 × 10<SUP>16</SUP>
  g and a total mass of 8.9 × 10<SUP>16</SUP> 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 × 10<SUP>17</SUP> g spread over much of the earthward
  facing hemisphere.

---------------------------------------------------------
Title: A Search for Early Optical Emission at Gamma-Ray Burst
    Locations by the Solar Mass Ejection Imager (SMEI)
Authors: Buffington, Andrew; Band, David L.; Jackson, Bernard V.;
   Hick, P. Paul; Smith, Aaron C.
2006ApJ...637..880B    Altcode: 2005astro.ph.10159B
  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.

---------------------------------------------------------
Title: Global 3-D Solar Wind Analysis of Halo CMEs Using
    Interplanetary Scintillation (IPS) Remote Sensing and its Comparison
    at Mars
Authors: Boyer, J. A.; Jackson, B. V.; Buffington, A.; Hick, P. P.;
   Yu, Y.; Crider, D. H.
2005AGUFMSH43A1145B    Altcode:
  The Interplanetary Scintillation (IPS) process allows observation
  of the inner heliospheric response to CMEs in scintillation level
  and velocity. With the help of our colleagues in STELab, Japan, we
  have developed near real time access of these data for use in space
  weather forecasting. We use a 3D reconstruction technique that obtains
  perspective views from outward-flowing solar wind as observed from
  Earth by iteratively fitting a kinematic solar wind model using the
  IPS observations. This 3D modeling technique permits us to reconstruct
  the density and velocity structure of CMEs, and other interplanetary
  transient structure at low resolution (with a one day cadence, and at a
  20 deg. latitudinal and longitudinal heliographic resolution). Here we
  explore the use of this technique to reproduce the solar wind pressure
  observed at Mars following the aftermath of halo (Earth-directed)
  CMEs. These CMEs include one that erupted from the Sun on May 27,
  2003 and another on October 28, 2003 both of which produced a large
  response at Mars. In addition we explore the response at Mars and our
  reconstruction of "backside" (as seen from Earth) halo CMEs.

---------------------------------------------------------
Title: Solar Mass Ejection Imager (SMEI) Solar Wind 3-D Analysis of
    the January 20, 2005 CME
Authors: Jackson, B. V.; Buffington, A.; Hick, P. P.; Yu, Y.; Webb, D.
2005AGUFMSH21A..02J    Altcode:
  The Solar Mass Ejection Imager (SMEI) has observed the inner
  heliospheric response in white light from over 200 CMEs. One of these,
  on January 20, 2005, produced one of the largest Solar Energetic
  Particle events ever recorded. We show SMEI orbital difference images
  and the 3D solar wind reconstruction of this well-observed CME, and
  demonstrate how we can track its outward motion from approximately 20
  deg. from the Sun until it vanishes in the SMEI field of view in the
  direction of the Ulysses spacecraft. Our 3D reconstruction technique
  is used to obtain perspective views from outward-flowing solar wind
  as observed from Earth by iteratively fitting a kinematic solar wind
  density model using the SMEI white light observations. This 3D modeling
  technique permits us to separate the heliospheric response in SMEI
  from background noise, and to estimate the 3D structure and transient
  heliospheric components of the CME and its speed and mass. We then
  determine the total energy of the CME that can be used as input to
  determine the total energy output of the event. More information about
  the spatial extent and energetics of this CME event can be determined
  by measurements in-situ from the Ulysses spacecraft that was beyond 5 AU
  and about 35 degrees west of Earth. Ulysses first detected an extremely
  fast CME response at the spacecraft 7 days following the event on the
  Sun and the transient flow continued for several days. The SMEI 3D
  reconstruction shows the event as it passes Earth to the west and helps
  to disentangle the CME structure. This will allow a better understanding
  of which portions of the CME intersect Ulysses, and the 3D trajectories
  of several CMEs observed earlier in coronagraph and SMEI data.

---------------------------------------------------------
Title: 3D CME Mass and Energy From Solar Mass Ejection Imager (SMEI)
    and Interplanetary Scintillation (IPS) Data
Authors: Jackson, B. V.; Buffington, A.; Hick, P. P.; Yu, Y.
2005AAS...20711108J    Altcode: 2005BAAS...37.1342J
  White-light Thomson scattering observations from the Solar Mass Ejection
  Imager (SMEI) have recorded the inner heliospheric response to several
  hundred CMEs including the halo CMEs of May 28, 2003 and October 28,
  2003, and numerous other heliospheric structures. We show the extent
  of several well-observed CMEs in SMEI observations, and measure these
  events from their first observations in SMEI approximately 20 degrees
  from the solar disk until they vanish in the SMEI field of view. Several
  portions of large CMEs can be observed in the interplanetary medium
  associated with the initial coronal response and the underlying
  erupting prominence structure observed by the LASCO coronagraphs
  and other instruments. To enhance the images and understand the
  outward propagation of these structures we use a 3D reconstruction
  technique that obtains perspective views from outward-flowing solar
  wind as observed from Earth, iteratively fitting a kinematic solar wind
  density model to the SMEI white light observations and, when available,
  also to the Solar-Terrestrial Environment Laboratory (STELab), Japan
  interplanetary scintillation (IPS) velocity data. This 3D modeling
  technique allows separating the heliospheric response in SMEI from
  background noise, and estimating the 3D structure of the CME and its
  mass. Pixel-to-pixel 3D comparison with the IPS velocity structure
  gives the outward flow kinetic energy for these events.

---------------------------------------------------------
Title: SMEI: A Spaceborne Observatory for Heliospheric Remote Sensing
Authors: Hick, P.; Jackson, B. V.; Buffington, A.; Yu, Y.
2005AGUFMSH51C1219H    Altcode:
  The Solar Mass Ejection Imager (SMEI) provides measurements of the
  Thomson scattering brightness with near-full sky coverage from Earth
  orbit. These observations allow three-dimensional reconstruction of the
  solar wind density and velocity throughout the inner heliosphere. We
  discuss how these observations provide context for in situ solar wind
  observations from other "Great Observatory" satellites near Earth
  (ACE), other planets (Mars Orbiter) and in deep space (Ulysses).

---------------------------------------------------------
Title: Coronal mass ejection kinematics deduced from white light
    (Solar Mass Ejection Imager) and radio (Wind/WAVES) observations
Authors: Reiner, M. J.; Jackson, B. V.; Webb, D. F.; Mizuno, D. R.;
   Kaiser, M. L.; Bougeret, J. -L.
2005JGRA..110.9S14R    Altcode: 2005JGRA..11009S14R
  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°, was
  observed by the Mauna Loa and Solar and Heliospheric Observatory
  (SOHO) Large-Angle Spectrometric Coronograph (LASCO) coronagraphs
  to 14 R<SUB>⊙</SUB>. The measured plane-of-sky speed of the LASCO
  CME was 2600 km s<SUP>-1</SUP>. 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.

---------------------------------------------------------
Title: Interactive visualization of solar mass ejection imager (SMEI)
    volumetric data
Authors: Yu, Yang; Hick, P. P.; Jackson, Bernard V.
2005SPIE.5901..335Y    Altcode:
  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.

---------------------------------------------------------
Title: Space performance of the multistage labyrinthine SMEI baffle
Authors: Buffington, Andrew; Jackson, Bernard V.; Hick, P. P.
2005SPIE.5901..325B    Altcode:
  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°. 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<SUP>-15</SUP> of surface-brightness reduction is
  required relative to the solar disk. The SMEI labyrinthine baffle
  provides roughly 10<SUP>-10</SUP> 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.

---------------------------------------------------------
Title: Low resolution three dimensional reconstruction of CMEs using
    solar mass ejection imager (SMEI) data
Authors: Jackson, Bernard V.; Buffington, Andrew; Hick, P. P.; Wang,
   Cindy X.
2005SPIE.5901....1J    Altcode:
  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° from the solar disk until they fade away
  in the SMEI 180° 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.

---------------------------------------------------------
Title: The SMEI real-time data pipeline: from raw CCD frames to
    photometrically accurate full-sky maps
Authors: Hick, P.; Buffington, A.; Jackson, B. V.
2005SPIE.5901..340H    Altcode:
  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.

---------------------------------------------------------
Title: Very high altitude aurora observations with the Solar Mass
    Ejection Imager
Authors: 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.
2005JGRA..110.7230M    Altcode: 2005JGRA..11007230M
  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 (≥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.

---------------------------------------------------------
Title: Power System for the Herschel &amp; Planck Spacecraft
Authors: Jackson, Bernard; Rueda, Pablo
2005ESASP.589E..66J    Altcode:
  Herschel and Planck are two scientific spacecraft missions of the
  European Space Agency. Herschel is a far infra-red and submillimeter
  observatory, and Planck is a spacecraft for research into cosmic
  background radiation anisotropy. Both spacecraft are planned for
  launch in 2007 by a single Ariane 5 launcher from Kourou (French
  Guyana). They will separate after launch and transit to different
  orbits around 'L2'.Both spacecraft feature common power sub systems
  with the only significant difference being the Solar Arrays (SA) where
  Planck will have a circular, body mounted array and Herschel a fixed
  panel array. Because the Solar Arrays also act as sunshields, and no
  heat can be emitted on the rear side, this leads to high SA operation
  temperatures.Also both spacecraft have instruments working close to
  zero Kelvin and this leads to particular design constraints for the
  spacecraft and in particular the power subsystem.Apart from the SAs
  the power management and distribution systems on the two spacecraft
  are identical. An Industrial Team with Alcatel Space Industries (F)
  as its prime, and involving Alenia Spazio S.p.A. (I) and Astrium GmbH
  (D) are leading the work.

---------------------------------------------------------
Title: Preliminary Three Dimensional CME Mass and Energy Using Solar
    Mass Ejection Imager (SMEI) Data
Authors: Jackson, B. V.; Buffington, A.; Hick, P. P.; Yu, Y.; Webb,
   D.; Mizuno, D.; Kuchar, T.
2005AGUSMSP44A..05J    Altcode:
  White-light Thomson scattering observations from the Solar Mass Ejection
  Imager (SMEI) have recorded the inner heliospheric response to several
  hundred CMEs including the May 28, 2003 halo CME, the October 28,
  2003 halo CME, and numerous other heliospheric structures. Here we
  show the extent of several well-observed CMEs in SMEI observations,
  and show how we are able to track events from their first measurements
  in SMEI approximately 20° from the solar disk until they vanish from
  the SMEI 180° field of view. Several portions of large CMEs observed
  by the LASCO coronagraphs can be tracked into the interplanetary
  medium associated with the initial CME response and the underlying
  erupting prominence structure. We use a 3D reconstruction technique
  that obtains perspective views from outward-flowing solar wind as
  observed from Earth, iteratively fitting a kinematic solar wind density
  model using the SMEI white light observations and, when available, the
  Solar-Terrestrial Environment Laboratory (STELab), Japan interplanetary
  scintillation (IPS) velocity data. This 3D modeling technique allows
  us to separate the heliospheric response in SMEI from background noise,
  and to estimate the 3D structure of the CME and its mass. For instance,
  the analysis shows and tracks outward the northward portion of the loop
  structure of the October 28, 2003 CME observed as a halo in LASCO images
  that passes Earth on October 29. We determine an excess mass for this
  structure of 6.7×1016g and a total mass including an ambient background
  of 8.3×1016g. The very fast structure compared in a 3D pixel to pixel
  comparison with the IPS velocity data gives a kinetic energy for the
  northward portion of this event of 2.0×1034erg as it passes Earth.

---------------------------------------------------------
Title: Comparative Analyses of the CSSS Calculation in the UCSD
    Tomographic Solar Observations
Authors: Dunn, T.; Jackson, B. V.; Hick, P. P.; Buffington, A.; Zhao,
   X. P.
2005SoPh..227..339D    Altcode:
  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 15R<SUB>⊙</SUB>. 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.

---------------------------------------------------------
Title: Three-dimensional structure of compound interplanetary
    transients associated with 27-28 May 2003 coronal mass ejections
Authors: Tokumaru, M.; Kojima, M.; Fujiki, K.; Yamashita, M.; Jackson,
   B. V.; Hick, P.
2004AGUFMSH11A..01T    Altcode:
  We have investigated the global features of interplanetary (IP)
  disturbances associated with 27-28 May coronal mass ejection (CME)
  events using interplanetary scintillation (IPS) measurements of
  the Solar-Terrestrial Environment Laboratory (STEL). Our IPS data
  taken between 2003 May 28 22h UT and May 29 7h UT showed a set of
  complex feature of IP disturbances, and most of them are regarded as
  IP consequences of two full-halo CMEs which occurred in association
  with the X1.3/2B flare on May 27 23:07 UT and the X3.3 flare on May 28
  00:27 UT. Some components of the IP disturbances were discriminated from
  the IPS data by making the model fitting analysis iteratively. One of
  the components was an Earth-directed one, which appears to correspond
  to the IP shock observed by ACE on May 29 18:30 UT. Other components
  were obliquely propagating ones, which either preceded or followed the
  Earth-directed one. The global features deduced here are generally
  in agreement with heliospheric reconstructions made from Solar Mass
  Ejection Imager (SMEI) measurements.

---------------------------------------------------------
Title: Heliospheric Photometric Images and 3D Reconstruction from
    the Solar Mass Ejection Imager (SMEI) Data
Authors: Jackson, B. V.; Buffington, A.; Hick, P. P.
2004AGUFMSH11A..02J    Altcode:
  The Solar Mass Ejection Imager (SMEI) experiment is fixed to
  the Coriolis spacecraft and views the sky above Earth using
  sunlight-rejecting baffles and CCD camera technology. SMEI was
  designed to provide precise photometric white light images over most
  of the sky on each 102-minute Earth orbit. The brightness sky maps
  of the inner heliosphere indicate a rich variety of electron density
  structures that are produced by the material that propagates through
  it and its interaction with ambient structures. We present some of
  the preliminary results of the analysis of these photometric SMEI
  observations derived by modeling the white light observations such
  that most of the contaminant signals: stars, the zodiacal cloud and
  high-energy particle variations are removed. We will also show some
  of the 3D reconstructions that allow this contaminant signal removal
  using both interplanetary scintillation (IPS) and SMEI data.

---------------------------------------------------------
Title: Preliminary Three Dimensional Reconstruction of CMEs Using
    Solar Mass Ejection Imager (SMEI) Data
Authors: Jackson, B. V.; Buffington, A.; Hick, P. P.; Wang, X.
2004AAS...205.4305J    Altcode: 2004BAAS...36.1412J
  White-light Thomson scattering observations from the Solar Mass Ejection
  Imager (SMEI) have recorded the inner heliospheric response to the
  October 28, 2003 CME. Here we detail the extent of this particular
  CME event in SMEI observations, and we show how we are able to track
  the event from its first measurement approximately 20<SUP>o</SUP>
  from the solar disk until it fades away in the SMEI 180<SUP>o</SUP>
  field of view. Several portions of this CME that can be tracked
  into the interplanetary medium are associated with the initial
  CME response and the underlying erupting prominence structure. We
  employ a 3D reconstruction technique that provides perspective views
  from outward-flowing solar wind as observed from 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. The preliminary SMEI white light calibration indicates
  a total mass of 6 X 10<SUP>16</SUP>g for the ejecta associated
  with the prominence eruption. The total mass of this CME including
  possible associated nearby structures may have been as much as 2 X
  10<SUP>17</SUP>g of inner heliospheric response spread over much of
  the Earthward-facing hemisphere.

---------------------------------------------------------
Title: The Deceleration of Interplanetary Transients Between the
    Sun and 5 AU
Authors: Tappin, J.; Simnett, G. M.; Jackson, B. V.
2004AGUFMSH21A0394T    Altcode:
  During the the SMEI mission, Ulysses has been at relatively low
  latitudes (less than 25 degrees) and near aphelion (4.8 to 5.4 AU). This
  has provided us with an opportunity to trace interplanetary transient
  disturbances from near the Sun (with LASCO), around 1AU with SMEI and
  ACE and then again near 5AU with Ulysses. We have selected a number of
  events where the identification of the disturbance is clear in LASCO,
  SMEI and Ulysses and use the propagation of the disturbance through
  the heliosphere to draw conclusions regarding the dynamics of these
  disturbances. In particular we focus on the duration of the "driving
  flow" and on the significance of "swept-up" matter.

---------------------------------------------------------
Title: Wind/WAVES and SMEI Observations of ICMEs
Authors: Reiner, M. J.; Jackson, B. V.; Webb, D. F.; Kaiser, M. L.;
   Cliver, E. W.; Bougeret, J. L.
2004AGUFMSH11A..05R    Altcode:
  The low-frequency (kilometric) radio observations on Wind/WAVES
  provide important spectral and directional information related to the
  propagation of ICMEs through interplanetary space. However, up to now
  there has been no white-light observations with which to compare these
  low-frequency interplanetary radio observations, beyond the 30 Rs limit
  of the LASCO field of view. The recently launched Air Force Coriolis
  spacecraft that includes the Solar Mass Ejection Imager (SMEI), which
  is the first all-sky camera designed to track ICMEs from the Sun to
  1 AU, provides a unique opportunity of simultaneously tracking CMEs,
  both in white light and in radio, all the way from the corona to 1
  AU. 3D reconstruction techniques, utilizing multiple perspective views
  of the ICME observed by SMEI, represent the propagation and evolution
  of these density structures through the 3D heliosphere. There are two
  general ways that the Wind/WAVES radio data can be directly related
  to the SMEI heliospheric white-light observations. First, since
  the observed radio frequency depends on the local plasma density in
  the radio source region and since the interplanetary plasma density
  falls off with the inverse of the heliocentric distance squared, the
  observed radio frequency generated by the CME/shock decreases as the
  type II radio source associated with the CME propagates farther from the
  Sun. Thus the frequency characteristics of the type II radio emissions
  provide information on the radial distance of the ICME. Secondly, the
  low-frequency radio receivers on the Wind spacecraft have the unique
  capability of providing information on the direction of arrival of the
  radio emissions and of the size of the radio-emitting region. Both
  of these results, obtained from analyses of the Wind/WAVES radio
  observations, will be directly compared with the results from the
  analyses of the SMEI white-light data for various ICME events.

---------------------------------------------------------
Title: Comparison of Solar Mass Ejection Imager (SMEI) White Light
    Observations with IPS Velocity
Authors: Jackson, B. V.; Buffington, A.; Hick, P. P.; Kojima, M.;
   Tokumaru, M.
2004AGUFMSH21A0393J    Altcode:
  The Solar Mass Ejection Imager (SMEI) experiment is fixed
  to the Coriolis spacecraft and views the sky above Earth using
  sunlight-rejecting baffles and CCD camera technology. SMEI was designed
  to provide precise photometric white light images over most of the sky
  on each 102-minute Earth orbit. The brightness sky maps of the inner
  heliosphere indicate a rich variety of electron density structures
  that are produced by the material that propagates through it and its
  interaction with ambient structures. We present some of the preliminary
  results of the analysis of these photometric SMEI observations derived
  by 3D reconstructions that allow contaminant signal removal using both
  interplanetary scintillation (IPS) velocities and SMEI data. We use
  these analyses to compare preliminary SMEI tomographic white-light
  results with IPS velocity for the same time intervals.

---------------------------------------------------------
Title: Systematic Error Reduction and Photometric Calibration for
    the Solar Mass Ejection Imager (SMEI)
Authors: Buffington, A.; Jackson, B. V.; Hick, P.
2004AGUFMSH11A..07B    Altcode:
  The Solar Mass Ejection Imager (SMEI) instrument provides white-light
  photometric maps covering most of the sky each orbit of the Coriolis
  spacecraft. The SMEI differential photometry specification is 0.1% for
  each 1 square degree sky bin. A labyrinthine baffle reduces scattered
  sunlight, but for a portion of the data a background residue must also
  be subtracted to finally reach this specification. We describe this
  process, and further discuss how bright stars are used to determine an
  appropriate conversion from the CCD-camera data units to sky surface
  brightness. Also, the CCD in the camera viewing closest to the Sun
  operates significantly warmer than expected, which gives rise to
  a changing population of "hot pixels". We describe a data-analysis
  process which significantly alleviates the photometric impact of this.

---------------------------------------------------------
Title: Photometric Calibration for the Solar Mass Ejection Imager
    (SMEI)
Authors: Buffington, A.; Smith, A. C.; Jackson, B. V.; Hick, P. P.
2004AAS...205.1007B    Altcode: 2004BAAS...36.1350B
  The Solar Mass Ejection Imager (SMEI) was designed to record a
  photometric white-light response of the interplanetary medium from
  Earth over most of the sky in near real time, using Thomson scattered
  sunlight. In its first two years the instrument has observed several
  hundred Coronal Mass Ejections. Quantitative interpretations of these
  data requires that the Analog Data Units (ADUs) of the instrument's CCD
  responses be converted to an effective stellar brightness. The present
  work provides a preliminary report on establishing this relationship. <P
  />An appropriate unit here is an "S10", the equivalent brightness of
  a 10th magnitude star spread over one square degree. The relationship
  between ADUs and S10s is established by using the SMEI response to
  bright stars having known visual magnitude and spectral type. These
  latter are converted to a "SMEI magnitude" by integrating the various
  star's spectra over the nominal SMEI bandpass, which extends between
  0.4 and 1.1 microns and peaks at 0.7 microns, to obtain a spectral
  scaling factor which is set to unity for G-type stars and relates
  visual magnitudes to SMEI magnitudes. The final overall conversion
  factor is then determined from the ADU measurements of the individual
  stars. <P />This work was supported in part by NSF contract ATM0331513
  and NASA grant NAG 5-134543.

---------------------------------------------------------
Title: Near Real-Time Photometric Data Processing for the Solar Mass
    Ejection Imager (SMEI)
Authors: Hick, P. P.; Buffington, A.; Jackson, B. V.
2004AAS...205.1006H    Altcode: 2004BAAS...36.1350H
  The Solar Mass Ejection Imager (SMEI) records a photometric white-light
  response of the interplanetary medium from Earth over most of the sky
  in near real time. In the first two years of operation the instrument
  has recorded the inner heliospheric response to several hundred CMEs,
  including the May 28, 2003 and the October 28, 2003 halo CMEs. In
  this preliminary work we present the techniques required to process
  the SMEI data from the time the raw CCD images become available to
  their final assembly in photometrically accurate maps of the sky
  brightness relative to a long-term time base. <P />Processing of the
  SMEI data includes integration of new data into the SMEI data base; a
  conditioning program that removes from the raw CCD images an electronic
  offset ("pedestal") and a temperature-dependent dark current pattern; an
  "indexing" program that places these CCD images onto a high-resolution
  sidereal grid using known spacecraft pointing information. At this
  "indexing" stage further conditioning removes the bulk of the the
  effects of high-energy-particle hits ("cosmic rays"), space debris
  inside the field of view, and pixels with a sudden state change
  ("flipper pixels"). <P />Once the high-resolution grid is produced,
  it is reformatted to a lower-resolution set of sidereal maps of sky
  brightness. From these sidereal maps 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. Common formats are Sun-centered
  Hammer-Aitoff or "fisheye" maps. Time series at selected locations
  on these maps are extracted and processed further to remove aurorae,
  variable stars and other unwanted signals. These time series (with a
  long-term base removed) are used in 3D tomographic reconstructions. <P
  />The data processing is distributed over multiple PCs running Linux,
  and, runs as much as possible automatically using recurring batch jobs
  ('cronjobs'). The batch scrips are controlled by Python scripts. The
  core data processing routines are written in several computer languages:
  Fortran, C++ and IDL.

---------------------------------------------------------
Title: Interactive Visualization of Solar Mass Ejection Imager (SMEI)
    Volumetric Data
Authors: Wang, X.; Hick, P. P.; Jackson, B. V.
2004AAS...205.1005W    Altcode: 2004BAAS...36.1350W
  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 CME volumes and
  masses. In these visualizations we highlight two time periods where
  halo CMEs were observed by SMEI to engulf Earth, on May 30, 2003 and
  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.

---------------------------------------------------------
Title: Zodiacal Light Analysis and Removal From the Solar Mass
    Ejection Imager (SMEI) Data
Authors: Simon, S.; Jackson, B. V.; Buffington, A.; Hick, P. P.;
   Smith, A.
2004AGUFMSH21A0398S    Altcode:
  The Solar Mass Ejection Imager (SMEI) experiment provides white-light
  photometric maps covering most of the sky each orbit of the Coriolis
  spacecraft. The SMEI differential photometry specification is
  0.1% for each 1 square degree sky bin, and was designed to provide
  precise photometric white light images over most of the sky on each
  102-minute Earth orbit in order to map heliospheric structures. One of
  the brightest contaminant signals observed in SMEI is zodiacal light
  brightness that must be modeled and subtracted from the data in order
  to provide heliospheric sky maps free from large background changes. We
  have devised a technique to remove zodiacal dust brightness from the
  SMEI maps, and in order to do so accurately measure the asymmetry of
  the equatorial dust to the ecliptic plane as well as the Gegenschein
  brightness throughout the year. We present preliminary analyses of
  these observations for specific intervals during the one and a half
  year lifetime of SMEI.

---------------------------------------------------------
Title: The Solar Mass-Ejection Imager (SMEI) Mission
Authors: 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.
2004SoPh..225..177J    Altcode:
  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<SUP>∘</SUP>
  to greater than 90<SUP>∘</SUP> 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.

---------------------------------------------------------
Title: Three-Dimensional Tomography of Interplanetary Disturbances
Authors: Jackson, Bernard V.; Hick, P. Paul
2004ASSL..314..355J    Altcode:
  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.

---------------------------------------------------------
Title: The Solar Mass Ejection Imager (SMEI) and Its Potential as
    a Precision Time-Series Photometer
Authors: Buffington, A.; Jackson, B. V.; Hick, P. P.; Penny, A.
2004AAS...204.6910B    Altcode: 2004BAAS...36..795B
  The Solar Mass Ejection Imager (SMEI) was launched in January 2003
  into Earth orbit. SMEI is designed to observe heliospheric structures
  illuminated by Thomson-scattered sunlight. The design specification for
  SMEI is 0.1% in differential photometry for bright unresolved objects,
  to enable star removal from the heliospheric maps. Such a near-Earth
  imager will also provide photometric time-series measurements of these
  stars as a by-product of this removal process. For each 101-minute
  orbit, SMEI will deliver near complete sky maps having an expected
  (1 sigma) photometric resolution of about the equivalent of an
  11th magnitude star in a square degree. We will report on progress
  in establishing the photometric calibrations for the SMEI cameras,
  and discuss SMEI's potential for delivering photometric time-series
  measurements, which data can then be applied to the study of variable
  stars, eclipsing stellar systems, and to search for extrasolar planets
  by the occultation method.

---------------------------------------------------------
Title: The Solar Mass Ejection Imager (SMEI) Mission
Authors: Jackson, B. V.; Buffington, A.; Hick, P. P.; Kuchar, T.;
   Mizuno, D.; Webb, D. F.
2004AAS...204.1809J    Altcode: 2004BAAS...36..684J
  The Solar Mass Ejection Imager (SMEI) was launched in January 2003
  into Earth orbit. It observes sunlight that has Thomson-scattered from
  heliospheric structures of time-varying density. SMEI is designed to
  observe heliospheric structures such as coronal mass ejections (CMEs),
  corotating structures and shock waves to elongations greater than 90
  degrees from the Sun. Such a near-Earth imager can provide up to three
  days warning of the arrival of a CME 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 3D reconstructions of the heliospheric structures
  that it observes. We show images of several CMEs observed with this
  instrument and low-resolution reconstruction analyses using the SMEI
  data for each event. The 3D reconstructions and heights for these
  events are compared with elongation-time plots of the same CMEs to
  estimate true speeds and line-of-sight locations for each CME.

---------------------------------------------------------
Title: Coronal Mass Ejection Masses From CMEs Identified in
    Interplanetary Scintillation (IPS) Tomography and LASCO Coronagraph
    Images
Authors: Rappoport, S. A.; Jackson, B. V.; Hick, P. P.; Buffington,
   A.; Vourlidas, A.
2004AAS...204.3802R    Altcode: 2004BAAS...36..712R
  To optimize the information from individual radio source observations
  of the sky covering large elongations, we have developed a
  Computer-Assisted Tomography (CAT) program. We fit STELab (Nagoya
  University, Japan) interplanetary scintillation (IPS) observations to a
  time-dependent, three-dimensional heliospheric model. These observations
  allow us to create "sky maps" covering 10 to 80 degrees in elongation,
  in which we can track CMEs observed earlier in LASCO coronagraph
  images. These events have approximately the same shapes and extents as
  observed closer to the Sun. Here we map several CMEs in 3-dimensions as
  they move outward to 1 AU. Masses for each of the events are determined
  from the reconstruction analysis and are compared with plane of the
  sky masses obtained from calibrated LASCO coronagraph images.

---------------------------------------------------------
Title: Comparative analyses of the CSSS magnetic field calculation
    in the Univ. of California/San Diego tomographic solar wind model
    with in situ spacecraft observations
Authors: Dunn, Tamsen; Hick, P. P.; Jackson, Bernard V.; Buffington,
   Andrew; Zhao, Xue Pu
2004SPIE.5171....6D    Altcode:
  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

---------------------------------------------------------
Title: Visualization of remotely sensed heliospheric plasmas for
    space weather applications
Authors: Wang, Xin; Hick, P. P.; Jackson, Bernard V.; Bailey, Mike
2004SPIE.5171..280W    Altcode:
  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.

---------------------------------------------------------
Title: SMEI: design and development of an Earth-orbiting all-sky
    coronagraph
Authors: Jackson, Bernard V.; Hick, P. P.; Buffington, Andrew; Gold,
   Robert E.; Simnett, George M.; Eyles, Christopher J.; Cooke, Mark P.;
   Waltham, Nicholas R.
2004SPIE.5171....1J    Altcode:
  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.

---------------------------------------------------------
Title: Heliospheric tomography: an algorithm for the reconstruction
    of the 3D solar wind from remote sensing observations
Authors: Hick, P. P.; Jackson, Bernard V.
2004SPIE.5171..287H    Altcode:
  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.

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Title: Tracking a major interplanetary disturbance with SMEI
Authors: 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.
2004GeoRL..31.2802T    Altcode: 2004GeoRL..3102802T
  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.

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Title: IPS From LOFAR: A Complement to Thomson Scattering Studies
Authors: Oberoi, D.; Kasper, J. C.; Lonsdale, C. J.; Salah, J. E.;
   Lazarus, A. J.; Jackson, B. V.
2003AGUFMSH41B0463O    Altcode:
  Information about the large scale physical properties of the inner
  heliosphere plasma can only be obtained by employing remote sensing
  techniques. The two most useful measurement techniques for this
  are Thomson scattering, used by Solar Mass Ejection Imager (SMEI),
  and Interplanetary Scintillation (IPS). Both these techniques
  are sensitive to the distribution of properties of the solar wind
  plasma along the entire line-of-sight through the medium. The two
  measurement techniques are sensitive to different properties of the
  same physical plasma. IPS is sensitive to the fluctuations in the
  refractive index of the medium (~ δ n<SUB>e<SUP>2</SUP></SUB>) and
  their spectral index, the perpendicular component of velocity of the
  solar wind, the anisotropy in electron density fluctuations caused
  by the magnetic field and their inner scale. Thomson scattering, on
  the other hand, is sensitive only to the distribution of the electron
  density along the line of sight. The data from both these techniques are
  suitable for tomographic reconstructions, yielding three dimensional
  visualisations of the inner heliosphere. Heliospheric tomography will
  benefit significantly from the denser sky coverage and the improved
  signal-to-noise IPS measurements promised by the upcoming instruments
  and the simultaneous use of Thomson scattering data. The unquestionable
  synergy between the information obtained from these two techniques
  should be exploited to arrive at significantly better constrained
  tomographic reconstructions. We are now assessing the potential for
  space weather applications, including IPS studies, of the Low Frequency
  Array (LOFAR), an aperture synthesis radio interferometer covering
  the 10-240 MHz range. The unique design of this instrument allows
  the possibility of high sensitivity observations of up to 4000 IPS
  sources a day. This unprecedented ability will increase the sampling
  of the inner heliosphere by ∼2 orders of magnitude compared to the
  present IPS instruments and improve the signal-to-noise of individual
  measurements. This paper will describe some aspects of the LOFAR design
  and outline its potential IPS measurement capabilities.

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Title: SMEI: First Results and Future Capabilities
Authors: Webb, D. F.; Mozer, J. B.; Radick, R. R.; Johnston, J. C.;
   Price, S. D.; Kuchar, T.; Mizuno, D. R.; Jackson, B. V.; Buffington,
   A.; Tappin, S. J.; Simnett, G. M.
2003AGUFMSH41C..03W    Altcode:
  The Solar Mass Ejection Imager (SMEI) experiment was launched on the
  STP Coriolis mission 6 January 2003 and is now recording all-sky,
  white light images on each 101-minute orbit. SMEI is fixed to the
  spacecraft and views the sky above Earth using sunlight-rejecting
  baffles and CCD camera technology. When fully calibrated, sky maps of
  structures having enhanced electron density in the inner heliosphere
  will be routinely produced. We will present some preliminary results
  of the early analysis of SMEI data. These include observations of
  several dozen coronal mass ejections (CMEs) as confirmed by the SOHO
  LASCO coronagraphs. One of these was a halo event which propagated to
  and beyond 1 AU and was associated with a major geomagnetic storm at
  Earth. Tomographic techniques are being developed to analyze the SMEI
  observations of the heliospheric plasma, including the transient CMEs
  and corotating interaction regions. SMEI also detected Comet NEAT
  inbound to and outbound from the Sun and the asteroid Vesta. With
  SMEI data we also can study solar and solar wind processes, and the
  experiment is capable of observing various other astronomical phenomena,
  such as variable stars, the Zodiacal light, near-Earth objects and
  extrasolar planetary transits.

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Title: The Solar Mass Ejection Imager (SMEI) Mission
Authors: Jackson, B. V.; Buffington, A.; Hick, P. P.; Holladay, P.;
   Johnston, J. C.; Kahler, S. W.; Mozer, J.; Price, S.; Radick, R. R.;
   Sinclair, D.; Simnett, G. M.; Eyles, C. J.; Cooke, M. P.; Tappin,
   J.; Waltham, N. R.; Kuchar, T.; Mizuno, D.; Webb, D. F.
2003AGUFMSH41B0457J    Altcode:
  We have designed, built and launched into near-Earth orbit a Solar
  Mass Ejection Imager (SMEI) capable of observing sunlight that
  has Thomson-scattered from heliospheric structures of time-varying
  density. SMEI is designed to observe heliospheric structures such
  as coronal mass ejections, corotating structures and shock waves,
  to elongations greater than 90° from the Sun. The instrument was
  inspired by the heliospheric imaging capability demonstrated by the
  zodiacal light photometers of the Helios spacecraft. The instrument
  makes effective use of in situ solar wind data from spacecraft in the
  vicinity of the imager by extending observations to the surrounding
  environment and back to the Sun. 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 tomographic analysis of the heliospheric structures
  surrounding it.

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Title: Space Performance of the Multistage Labyrinthine SMEI Baffle
Authors: Buffington, A.; Jackson, B. V.; Hick, P. P.
2003AGUFMSH41B0459B    Altcode:
  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-oriented CORIOLIS
  spacecraft cover most of the sky beyond about 20° from the Sun,
  each 102-minute orbit. Data from this instrument will ultimately
  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 will 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<SUP>-15</SUP> of surface-reduction is required
  relative to the solar disk. The SMEI labyrinthine baffle provides
  roughly 10<SUP>-10</SUP> of this reduction; the subsequent optics
  provides the remainder. We analyze data covering a range of angles
  between the SMEI optical axis and the Sun, or the Moon, to evaluate
  the full system's stray-light rejection performance.

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Title: The Solar Mass Ejection Imager (SMEI)
Authors: Simnett, G. M.; Eyles, C. J.; Cooke, M. P.; Waltham, N. R.;
   King, J. M.; Jackson, B. V.; Buffington, A.; Hick, P. P.; Holladay,
   P. E.; Anderson, P. A.
2003AGUFMSH41C..02S    Altcode:
  The Solar Mass Ejection Imager (SMEI) has been designed to detect and
  forecast the arrival of solar mass ejections and other heliospheric
  structures which are moving towards the Earth. We describe the
  instrument, which was launched into a Sun-synchronous polar orbit
  on 6 January, 2003 on board the US DoD Coriolis spacecrafth. SMEI
  contains three CCD cameras, sensitive over the optical waveband,
  each with a field-of-view of 60 degrees x 3 degrees. The sensitivity
  is such that it will detect changes in sky brightness equivalent to
  a tenth magnitude star in one square degree of sky. Each camera takes
  an image every 4s and the normal telemetry rate is 128 kbits/s. SMEI
  has a photometric accuracy of around 0.1%. In addition to solar mass
  ejections, images of stars and the zodiacal cloud are measured to this
  photometric accuracy once/ orbit (102 minutes).

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Title: Stellar Variability Studies with SMEI
Authors: Penny, A. J.; Jackson, B. V.; Buffington, A.; Hick, P. P.;
   Kahler, S. W.; Price, S.; Johnston, J. C.; Holladay, P.; Sinclair,
   D.; Radick, R. R.; Mozer, J. C.; Anderson, P.; Simnett, G. M.; Eyles,
   C. J.; Cooke, M. P.; Tappin, J.; Waltham, N. R.; Kuchnar, T.; Mizuno,
   D.; Webb, D. F.
2003AGUFMSH41C..08P    Altcode:
  The Solar Mass Ejection Imager (SMEI) instrument images most of the sky
  every 105 minutes. From this unique dataset, the brightnesses of stars
  down to and below the eight magnitude can be measured to investigate
  their variability. This paper presents the methods developed to extract
  the stellar brightnesses, and the accuracies obtained as a function
  of brightness and crowding. Example lightcurves are given.

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Title: IPS/SMEI potential joint observations
Authors: Tokumaru, M.; Kojima, M.; Fujiki, K.; Jackson, B. V.; Hick, P.
2003AGUFMSH41C..05T    Altcode:
  Interplanetary scintillation (IPS) measurements are known as one
  of remote-sensing techniques which enable us to gain access to
  global features of the solar wind (e.g. quasi-stationary corotating
  structures, transient streams associated with CMEs). We have carried
  out a long-term collaboration on the reconstruction of the heliospheric
  features from IPS measurements made with the 327 MHz four-station
  system of the Solar-Terrestrial Environment Laboratory (STEL),
  Nagoya University. Under the collaboration, we have developed the
  computer-assisted tomography (CAT) analysis method, which allows us to
  retrieve the 3D distribution of the solar wind velocity and density
  from IPS data. We also have been making the real-time reconstruction
  experiment of heliospheric features using STEL IPS data and the CAT
  method. Based on these results, we propose here the joint observations
  of IPS and SMEI. The SMEI is a powerful tool to investigate the global
  heliospheric features, and its capability is complementary to one of
  IPS observations; That is, SMEI observations provide a high-resolution
  image of the solar wind density distribution, while IPS observations
  provide reliable estimates of the solar wind velocity. Therefore, a
  combination of IPS and SMEI observations is essential for achieving a
  precise reconstruction of global heliospheric (velocity and density)
  features by the CAT analysis.

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Title: Interactive Visualization of Transient Solar Wind Phenomena
    for Space Weather Applications
Authors: Wang, C. X.; Hick, P. P.; Jackson, B. V.
2003AGUFMSH41B0458W    Altcode:
  We present a volume rendering system developed for the visualization and
  manipulation of 3D heliospheric volume data such as solar wind density,
  velocity and magnetic field. Our system exploits the capabilities of
  the VolumePro 1000 board 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. Many operations
  have been implemented such as stereo/perspective views, animations
  of time-sequences, and determination of CME volumes and masses. We
  will show examples of three-dimensional heliospheric volumes from
  tomographic reconstructions of density and velocity using real-time
  interplanetary scintillation (IPS) data. In the near future we expect
  to add reconstructions based on the all-sky observations from the
  recently launched Solar Mass Ejection Imager and employ our system to
  interactively analyze and visualize the abundant information embedded
  in these data.

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Title: Recent Comparative Analyses of the CSSS UCSD Tomographic
    Solar Wind Model with in situ Spacecraft Observations
Authors: Dunn, T.; Hick, P.; Jackson, B. V.; Buffington, A.
2003AGUFMSH42B0526D    Altcode:
  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 are now becoming available from the
  Solar Mass Ejection Imager. We use solar surface magnetogram data,
  and a source surface provided by the Stanford Current-Sheet Source
  Surface model, to provide input to the UCSD tomography program. The
  UCSD tomography program extrapolates the magnetic field out to and
  beyond Earth. The latest results are compared with in situ data.

---------------------------------------------------------
Title: The Solar Mass Ejection Imager (Smei)
Authors: 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.
2003SoPh..217..319E    Altcode:
  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°×3°, 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<SUP>−1</SUP>. 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.

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Title: Time-dependent tomography of hemispheric features using
    interplanetary scintillation (IPS) remote-sensing observations
Authors: Jackson, B. V.; Hick, P. P.; Buffington, A.; Kojima, M.;
   Tokumaru, M.; Fujiki, K.; Ohmi, T.; Yamashita, M.
2003AIPC..679...75J    Altcode:
  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.

---------------------------------------------------------
Title: Time-dependent tomography of heliospheric structures using
    IPS and Thomson scattering observations
Authors: Jackson, Bernard V.; Hick, P. P.; Buffington, A.
2003ESASP.535..823J    Altcode: 2003iscs.symp..823J
  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).

---------------------------------------------------------
Title: Time-dependent tomography of heliospheric features using the
    three-dimensional reconstruction techniques developed for the solar
    mass ejection imager (SMEI)
Authors: Jackson, Bernard V.; Hick, Pierre P.; Buffington, Andrew
2003SPIE.4853...23J    Altcode:
  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.

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Title: Introduction of the CSSS magnetic field calculation into the
    UCSD tomographic solar wind model
Authors: Dunn, Tamsen; Hick, Pierre P.; Jackson, Bernard V.; Zhao,
   Xuepu
2003SPIE.4853..504D    Altcode:
  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
  (R<SUB>s</SUB>). The UCSD kinematic model convects magnetic field
  from 15 R<SUB>s</SUB> 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

---------------------------------------------------------
Title: Calculations for and laboratory measurements of a multistage
    labyrinthine baffle for SMEI
Authors: Buffington, Andrew; Jackson, Bernard V.; Hick, Pierre P.
2003SPIE.4853..490B    Altcode:
  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 degrees of the solar disk with
  a field of view 60° long by 3° wide. Placed end-to-end, three fields
  of view then cover a nearly 180° 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<SUP>-15
  </SUP>of surface-brightness reduction is required relative to the solar
  disk. The SMEI labyrinthine baffle provides roughly 10<SUP>-10 </SUP>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.

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Title: Tomography of Heliospheric Features Developed for Smei
Authors: Jackson, Bernard V.; Hick, P. P.; Buffington, Andrew
2003IAUJD...7E..23J    Altcode:
  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 as observed in Thomson
  scattering. The technique provides three-dimensional reconstructions of
  heliospheric density. 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).

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Title: The 3d Solar Wind Over the Solar Cycle Observed by IPS
Authors: Kojima, Masayoshi; Jackson, Bernard V.; Ohmi, Tomoaki; Hick,
   Paul; Hayashi, Keiji; Tokumaru, Munetoshi; Fujiki, Ken-Ichi
2003IAUJD...7E..25K    Altcode:
  The interplanetary scintillation (IPS) method can observe the dynamics
  and structure of the solar wind in three dimensions with a relatively
  short time cadence. Because IPS observations are line-of-sight
  integrations we have developed an IPS tomography analysis method that
  can retrieve three-dimensional solar wind parameters as well as provide
  better spatial resolutions than previous IPS techniques. Using the
  IPS tomography analysis we have studied the solar cycle dependence
  of the solar wind properties such as the velocity of fast solar wind
  bimodal structure north-south asymmetry of fast wind and the origin of a
  compact slow streamer. Solar wind structure is bimodal not only in the
  solar minimum phase but also in the ascending and descending phases;
  In solar minimum phase a small coronal hole in vicinity of an active
  region emanates slow wind and a polar coronal hole also becomes the
  source of slow wind when it shrinks to a small size at solar maximum;
  the velocity of the fast wind does not change significantly when
  a coronal hole changes its size in the descending and ascending
  phases. We also introduce the three-dimensional dynamic nature of
  interplanetary transient events that were observed with another new
  technique: time-dependent tomography.

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Title: Coronal Mass Ejections Identified in Interplanetary
    Scintillation (IPS) Tomography and in LASCO Coronagraph Images
Authors: Rappoport, S. A.; Hick, P. P.; Jackson, B. V.
2002AAS...201.8303R    Altcode: 2002BAAS...34.1242R
  Coronal mass ejections (CMEs), including halo CMEs, can be observed in
  interplanetary scintillation (IPS) data. To optimize the information
  from radio source observations, we model them using a time-dependent
  three-dimensional tomography program. We depict this heliospheric model
  as a series of "sky map" images that cover elongations extending from
  10 to 80 degrees. These IPS maps show CMEs observed earlier in the
  LASCO coronagraph images with approximately the same shapes and extents
  that were seen closer to the Sun. Here, a series of these CME events,
  including halo CMEs, are mapped as they move outward to distances as
  great as 1 AU.

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Title: Corotational Tomography of Heliospheric Features Using Global
    Thomson Scattering Data
Authors: Jackson, Bernard V.; Hick, P. Paul
2002SoPh..211..345J    Altcode:
  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.

---------------------------------------------------------
Title: Remote-Sensing of the Solar Wind: A Space Weather Application
Authors: Hick, P. P.; Rappoport, S. A.; Jackson, B. V.; Dunn, T.;
   Wang, C.
2002AAS...20114102H    Altcode: 2003BAAS...35Q.567H
  Remote sensing observations of the solar wind in the inner
  heliosphere fill an observational gap between near-Sun remote
  sensing and near-Earth in-situ data. We use heliospheric tomography
  to follow solar disturbances from Sun to Earth as the basis for a
  real-time space weather system. Over the past few years interplanetary
  scintillation observations from the Solar-Terrestrial Laboratory at
  Nagoya University, Japan, were the main source of data. In the near
  future Thomson scattering observations from the recently launched Solar
  Mass Ejection Imager (SMEI) will be added. <P />Here we show some recent
  developments in the visualization techniques used to process the volume
  data sets produced by the tomographic analyis: solar wind density,
  velocity and magnetic field. 3D visualization is based on an image
  rendering engine written in the IDL programming language. In addition,
  we use hardware-based volume rendering with the Volume Pro PCI board
  from TeraRecon. This board renders 4D volume data (three spatial, plus
  the time dimension) in real-time, allowing interactive manipulation
  of evolving (time-dependent) data sets. <P />This work was supported
  through NASA grant NAG5-9423 and Air Force MURI grant F49620-01-0359.

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Title: Visualization of Remotely-Sensed Heliospheric Plasmas
Authors: Bailey, M.; Hick, P. P.; Wang, C.; Jackson, B. V.;
   Buffington, A.
2002AGUFMSH21A0511B    Altcode:
  We demonstrate a software application designed for the display and
  real-time manipulation of 3D heliospheric volume data, such as solar
  wind density, velocity and magnetic field. The 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 several examples of three-dimensional
  heliospheric volume data derived from tomographic reconstructions based
  on heliospheric remote sensing observations of the heliospheric density
  and velocity structure (e.g. Thomson scattering and interplanetary
  scintillation observations). This work was supported through NASA
  grant NAG5-9423 and Air Force MURI grant F49620-01-0359.

---------------------------------------------------------
Title: Halo CME's - Will They Hit or Miss Earth?
Authors: Jackson, B. V.; Hick, P. P.; Buffington, A.
2002AGUFMSH21A0474J    Altcode:
  To optimize the information from maps of the sky that cover large
  elongations we have developed a Computer Assisted Tomography (CAT)
  program that models these using a time-dependent three-dimensional
  heliospheric model to fit Thomson scattering or STELab (Nagoya
  University) interplanetary scintillation (IPS) observations. The
  duration of a CME event (typically several days) imposes the restriction
  that the reconstruction model primarily uses outward solar wind motion
  to give perspective views of each point in space. The results to date
  are commensurate with the observational coverage, temporal and spatial
  resolution, and signal to noise available from the original data. We
  provide remote observer views of IPS-based reconstructions of halo
  CMEs also observed by the LASCO coronagraphs. We practice our modeling
  techniques by making these views available in real time to forecast
  halo CME Earth-arrival. Here we explore the locations and shapes of a
  few select halo CMEs and their three-dimensional velocity structure in
  order to determine whether they will hit or miss the Earth. This work
  is supported by NASA grant NAG5-8504 and AFOSR grant F49620-01-1-0054.

---------------------------------------------------------
Title: 3-D Tomography of Interplanetary Disturbances
Authors: Jackson, B. V.; Hick, P. P.; Buffington, A.
2002AAS...200.4910J    Altcode: 2002BAAS...34..723J
  We are developing tomographic techniques for analyzing remote sensing
  observations of heliospheric density and velocity as observed in
  Thomson scattering (e.g. by the Helios photometers) and interplanetary
  scintillation (IPS) observations. We have refined the program to
  enable us to analyze time-dependent phenomena, such as the evolution of
  corotating heliospheric structures and rapidly evolving events such as
  coronal mass ejections. We intend our analyses to be used with data from
  the future Solar Mass Ejection Imager (SMEI) experiment. We currently
  provide these analyses in real-time using IPS observations in order to
  forecast the arrival of corotating structures and CMEs at Earth. This
  work is supported by NASA grant NAG5-9423 and AFOSR grant F49620-01-0054

---------------------------------------------------------
Title: The Magnetic Structure of CMEs - a Brief Introduction
Authors: Jackson, B. V.
2002AAS...200.6501J    Altcode: 2002BAAS...34..751J
  Coronal magnetic fields are considered a key driver of Coronal Mass
  Ejections (CMEs). The interior regions of CMEs, including their
  associated prominences, often appear to erupt as ropes of coronal
  flux. In situ observations from space reveal that interplanetary
  CMEs (ICMEs) can be associated with strong, rotating magnetic fields
  (clouds) that can often be modeled as flux ropes. Both the internal
  fields of CMEs and their interaction with quasi-steady heliospheric
  magnetic structures influence their propagation and structural
  development. However, there is only indirect evidence that coronal
  magnetic fields directly power the CME eruption, or how or even if
  solar surface magnetic fields change in response to a CME. I will
  briefly review current observations of the relationship between
  magnetic fields and CMEs, and show the effects of their propagation
  through the interplanetary medium.

---------------------------------------------------------
Title: Tomographic Analysis of Solar Wind Structure Using
    Interplanetary Scintillation
Authors: Kojima, M.; Fujiki, K.; Tokumaru, M.; Ohmi, T.; Shimizu,
   Y.; Yokobe, A.; Jackson, B. V.; Hick, P. L.
2002swsm.conf...55K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Introduction of the CSSS Magnetic Field Model into the UCSD
    Tomographic Solar Wind Model
Authors: Dunn, T.; Hick, P. P.; Jackson, B. V.; Buffington, A.
2001AGUFMSH31A0701D    Altcode:
  Our time-dependent tomographic technique developed over the last few
  years provides a kinematic model of the solar wind. The model, which
  has one-day time steps, allows us to determine the large-scale three
  dimensional extent of solar disturbances and to forecast their arrival
  at Earth in real-time. We introduce magnetic field calculations from
  the Stanford Current-Sheet Source Surface model (Zhao and Hoeksema,
  1995) at the source surface of our kinematic model and extrapolate
  the magnetic field out beyond Earth. We show an animated version of
  the convected magnetic field, and compare results with in situ data
  near Earth. We wish to thank Dr. XuePu Zhao for providing software and
  input data for the Stanford Current-Sheet Source Surface model. This
  work is supported by AFOSR contract F49620-01-1-0360. References: Zhao,
  X. and J.T. Hoeksema, Prediction of the interplanetary magnetic field
  strength, J. Geophys. Res. 100, 19, 1995.

---------------------------------------------------------
Title: Space Weather Using Remote Sensing Data
Authors: Jackson, B. V.; Hick, P. P.; Buffington, A.; Dunn, T.;
   Rappoport, S.; Kojima, M.; Tokumaru, M.; Fujiki, K.; Yokobe, A.;
   Ohmi, T.
2001AGUFMSH31A0698J    Altcode:
  We are developing tomographic techniques for analyzing remote
  sensing observations of the coronal and heliospheric density and
  velocity structure as observed in Thomson scattering and also using
  interplanetary scintillation (IPS) observations. We have refined our
  program to enable us to analyze time-dependent phenomena, such as the
  evolution of co-rotating heliospheric structures and rapidly evolving
  events such as coronal mass ejections, as observed e.g. with the future
  Solar Mass Ejection Imager (SMEI) experiment. We currently provide
  heliospheric three-dimensional reconstructions in real-time using IPS
  observations from STELab, Nagoya University, Japan in order to forecast
  the arrival at Earth of CMEs. We compare these reconstructions modeled
  at Earth with ACE in-situ spacecraft data and show these analyses along
  with a goodness-of-fit criterion designed to certify the reconstructions
  and refine our technique. This work is supported by AFOSR contract
  F49620-01-1-0054 and NASA contract NAG5-8504. index.html&lt;/a&gt;

---------------------------------------------------------
Title: A Study of Interacting Plasma Phenomena Using the Tomographic
    3-Dimensional Reconstruction Techniques Developed for the Solar Mass
    Ejection Imager (SMEI)
Authors: Jackson, B. V.; Hick, P. P.
2001AGUFMSH11D..04J    Altcode:
  We are developing tomographic techniques for analyzing remote sensing
  observations of heliospheric density and velocity structure as
  observed in Thomson scattering (e.g. using the Helios photometer
  data) for eventual use with Solar Mass Ejection Imager (SMEI)
  observations. 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. This work is supported by NASA grant NAG5-8504 and AFOSR
  grant F49620-01-1-0054. &gt;http://casswww.ucsd.edu/solar/crew/bjackson
  /index.html&lt;/a&gt;

---------------------------------------------------------
Title: Study of ICME Structure Using LASCO White Light and STE Lab
    IPS Observations of Halo CMEs
Authors: Webb, D. F.; Tokumaru, M.; Jackson, B. V.; Hick, P. P.
2001AGUFMSH31A0700W    Altcode:
  As part of a long-term investigation of halo-like coronal mass ejections
  (CMEs) well observed in white light by the SOHO LASCO coronagraphs,
  we report on a study comparing our catalog of parameters and solar and
  solar wind associations of halo CMEs with interplanetary disturbances
  observed with the interplanetary scintillation (IPS) radio array of
  STE Lab in Japan. We have cataloged over 100 full halo CMEs observed
  by LASCO from 1996 through 2000. This period covers the first half
  of solar cycle 23 from activity minimum to maximum. Although the STE
  Lab observations are limited during each year, nearly all of these
  CMEs occurring during STE Lab observations were associated with IPS
  disturbances within a day or so following the halo CME onset time. We
  will present a summary of these comparisons, and will discuss how the
  combined data sets can be used to determine key parameters of the
  3D shape, structure and propagation of ICMEs. At STE Lab a program
  is used to find best-fit parameters automatically by matching model
  calculations to the observed IPS g-value (proportional to plasma
  density) data. At UCSD a tomographic program is used to reconstruct
  3D views of ICMEs using the IPS data in a reconstruction technique
  based on solar rotation and outward solar wind motion. This work is
  also pertinent for observations that will be available from the Solar
  Mass Ejection Imager (SMEI) experiment to be launched next year and,
  later, from the NASA STEREO mission.

---------------------------------------------------------
Title: Volume Rendering of Heliospheric Data
Authors: Hick, P. P.; Jackson, B. V.; Bailey, M. J.; Buffington, A.
2001AGUFMSH31A0699H    Altcode:
  We demonstrate some of the techniques we currently use for the
  visualization of heliospheric volume data. Our 3D volume data usually
  are derived from tomographic reconstructions of the solar wind density
  and velocity from remote sensing observations (e.g., Thomson scattering
  and interplanetary scintillation observations). We show examples of
  hardware-based volume rendering using the Volume Pro PCI board (from
  TeraRecon, Inc.). This board updates the display at a rate of up to 30
  frames per second using a parallel projection algorithm, allowing the
  manipulation of volume data in real-time. In addition, the manipulation
  of 4D volume data (the 4th dimension usually representing time) enables
  the visualization in real-time of an evolving (time-dependent) data
  set. We also show examples of perspective projections using IDL. This
  work was supported through NASA grant NAG5-9423.

---------------------------------------------------------
Title: A heliospheric imager for Solar Orbiter
Authors: Jackson, B. V.; Buffington, A.; Hick, P. P.
2001ESASP.493..251J    Altcode: 2001sefs.work..251J
  No abstract at ADS

---------------------------------------------------------
Title: Evidence for space weather at Mercury
Authors: Killen, R. M.; Potter, A. E.; Reiff, P.; Sarantos, M.;
   Jackson, B. V.; Hick, P.; Giles, B.
2001JGR...10620509K    Altcode:
  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 meteoritic 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 of 20 during this week, while the solar EUV flux measured by
  the scanning electron microscope (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.

---------------------------------------------------------
Title: Space Weather Using Remote Sensing Data
Authors: Jackson, B. V.; Hick, P.; Buffington, A.
2001AGUSM..SH22C05J    Altcode:
  We are developing tomographic techniques for analyzing remote sensing
  observations of the coronal and heliospheric density and velocity
  structure as observed in Thomson scattering (e.g. by the SOHO/LASCO
  coronagraph and Helios photometers) and interplanetary scintillation
  (IPS) observations. We have refined the program to enable us to
  analyze time-dependent phenomena, such as the evolution of corotating
  heliospheric structures and rapidly evolving events such as coronal mass
  ejections, as observed e.g. with the future Solar Mass Ejection Imager
  (SMEI) experiment. We currently provide the three-dimensional analyses
  in real-time using IPS observations in order to forecast the arrival
  of CMEs, and we intend to show these analyses at our display. This work
  is supported by AFRL grant F49620-01-1-0054 and NSF grant ATM-9819947.

---------------------------------------------------------
Title: Visualization of Remotely-Sensed Heliospheric Plasmas
Authors: Hick, P.; Jackson, B. V.; Buffington, A.; Bailey, M. J.
2001AGUSM..SH22C04H    Altcode:
  We are currently developing a tomographic approach for analyzing
  remote sensing observations of the coronal and heliospheric density
  and velocity structure (e.g. Thomson scattering and interplanetary
  scintillation observations). Parallel to the tomographic techniques
  we are developing the visualization tools required for displaying
  and manipulating the three-dimensional tomographic results. We use a
  common graphics interface language (OpenGL, supported through IDL),
  standard visual interfaces (pop-up menus, sliders, point-and-click
  methods) and standard hardware (PCs). The visualization should be
  capable of simultaneously displaying the tomographic density and
  velocity model and should allow the user to dynamically view the
  heliospheric model using any predefined flight path through the
  three-dimensional cube covered by the model. For real-time volume
  rendering we use a Mitsubishi Volume Pro PCI board. We present our
  current progress in this visualization effort. Further details can
  be found on http://casswww.ucsd.edu/solar/index.html. This work was
  supported through NASA grant NAG5-9423.

---------------------------------------------------------
Title: Three-Dimensional Solar Wind Modeling Using Remote-Sensing Data
Authors: Hick, P. P.; Jackson, B. V.
2001SSRv...97...35H    Altcode:
  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).

---------------------------------------------------------
Title: Certifying Stray-Light Rejection and Photometric Performance
    for "SMEI"
Authors: Buffington, A.; Jackson, B. V.; Hick, P.
2001AGUSM..SH22C03B    Altcode:
  The Solar Mass Ejection Imager (SMEI) is a collaborative project
  between the Air Force, UCSD/CASS, and the University of Birmingham,
  England. It will fly on the CORIOLIS spacecraft, scheduled for
  launch in September 2002. The platform provides a zenith-pointing,
  terminator orbit. SMEI's three CCD cameras, each viewing a 3 x 60
  degree swath of sky, will provide a visible-light map of nearly
  the entire sky each 100-minute orbit. The instrument is designed to
  deliver 0.1% differential photometry, and 10-15 orders of magnitude
  scattered-light reduction when viewing further than 20 degrees from the
  Sun. We present the results of laboratory measurements which certify
  that these specifications are met by the SMEI flight hardware. We will
  also present night-sky data taken with the SMEI prototype optics, and
  progress on normalizing, flat-field correcting, and registering the
  SMEI data into a standard sky coordinate frame. This work is supported
  by AFRL contract F19628-00-C-0029.

---------------------------------------------------------
Title: Certifying Stray-Light Rejection and Photometric Performance
    for SMEI
Authors: Buffington, A.; Jackson, B. V.; Hick, P. P.; Kuchar, T. A.
2000AAS...197.5103B    Altcode: 2000BAAS...32.1488B
  The Solar Mass Ejection Imager (SMEI) is a collaborative project
  between the Air Force, UCSD/CASS, and the University of Birmingham,
  England. It will fly on the CORIOLIS spacecraft, scheduled for launch
  at the end of 2001. The platform provides a zenith-pointing, terminator
  orbit. SMEI's three CCD cameras, each viewing a 3 x 60 degree swath
  of sky, will provide a visible-light map of nearly the entire sky
  each 100-minute orbit. The instrument is designed to deliver 0.1%
  differential photometry, and 10<SUP>-15</SUP> scattered-light
  reduction when viewing further than 20 degrees from the Sun. We
  present the results of laboratory measurements which certify that
  these specifications are met by the SMEI flight hardware. We will also
  present night-sky data taken with the SMEI prototype optics. This work
  is supported by AFRL contract F19628-00-C-0029.

---------------------------------------------------------
Title: Space Weather Using Remote Sensing Data
Authors: Jackson, B. V.; Hick, P. P.; Buffington, A.
2000AAS...197.3108J    Altcode: 2000BAAS...32.1448J
  We are developing tomographic techniques for analyzing remote sensing
  observations of the coronal and heliospheric density and velocity
  structure as observed in Thomson scattering (e.g. by the SOHO/LASCO
  coronagraph and Helios photometers) and interplanetary scintillation
  (IPS) observations. We have refined the program to enable us to
  analyze time-dependent phenomena, such as the evolution of co-rotating
  heliospheric structures and rapidly evolving events such as coronal
  mass ejections, as observed e.g. by the Helios photometers, and with
  the future Solar Mass Ejection Imager (SMEI) experiment. We currently
  provide these analyses in real-time using IPS observations in order
  to forecast the arrival of CMEs and other heliospheric structures at
  Earth. This work is supported by NASA grant NAG5-9423 and NSF grant
  ATM-9819947.

---------------------------------------------------------
Title: Visualization of Remotely-Sensed Heliospheric Plasmas
Authors: Hick, P. P.; Jackson, B. V.; Buffington, A.
2000AAS...197.5102H    Altcode: 2000BAAS...32.1488H
  We are currently developing a tomographic approach for analyzing
  remote sensing observations of the coronal and heliospheric density
  and velocity structure (e.g. Thomson scattering and interplanetary
  scintillation observations). Parallel to the development of the
  tomographic techniques we are developing the visualization tools
  required for displaying and manipulating the three-dimensional
  tomographic results. We use a common graphics interface language
  (OpenGL, supported through IDL), standard visual interfaces (pop-up
  menus, sliders, point-and-click methods) and standard hardware
  (PCs). The visualization will target a software system capable of
  simultaneously displaying the tomographic density and velocity model
  (and, when available, magnetic field) and will allow the user to
  dynamically view the heliospheric model using any predefined flight
  path through the three-dimensional cube covered by the model, possibly
  using stereographics to get a better feel for the three-dimensionality
  of the model. Results of this ongoing visualization project
  will be demonstrated on a dedicated web site accessible through
  http://casswww.ucsd.edu/solar/index.html. This work was supported
  through NASA grant NAG5-9423.

---------------------------------------------------------
Title: Astronomy with SMEI
Authors: Kuchar, T. A.; Price, S. D.; Buffington, A.; Hick, P. P.;
   Jackson, B. V.
2000AAS...197.5101K    Altcode: 2000BAAS...32.1488K
  The Solar Mass Ejection Imager (SMEI) is comprised of three detectors
  capable of imaging coronal mass ejections (CMEs) from the Sun. It will
  orbit in an 830 km sun-synchronous orbit and provide a hemispherical
  view about the sun approximately every 100 minutes. The bandpass of
  the detectors is in the visual and near IR and ranges from 400 to
  1100 nm. The processed images will have a resolution of 1 degree in
  science data mode. The detection of CMEs will follow after the stellar
  background and other known astronomical phenomena (e.g. planets,
  asteroids, and zodiacal emission) have been registered and removed
  from the SMEI data. Since CMEs evolve on timescales of hours to days,
  data from a series of consecutive orbits can be compared to show their
  presence. The SMEI mission is scheduled to last for 5 years and thus
  has the potential to reveal variations on annual timescales. The data
  are uniquely suited to provide analysis for zodiacal background models
  over this wavelength range. In this poster we present the methodology
  for removing the stellar contribution from the SMEI data and how this
  can be used to track annual changes seen in the zodiacal cloud. We
  show a test of concept in this presentation using data taken with a
  prototype SMEI camera at the Table Mountain Observatory. SMEI is a
  collaborative project between the US Air Force, UCSD/CASS, and the
  University of Birmingham, England.

---------------------------------------------------------
Title: The Solar Mass Ejection Imager Optics and Baffles: Design
    and Construction
Authors: Jackson, Bernard V.; Buffington, Andrew; Hick, P. P.
2000STIN...0226912J    Altcode:
  The purpose of SMEI is a proof-of-concept of the ability to predict
  geomagnetic disturbances for Air Force space operations and to
  establish the feasibility of tracking interplanetary disturbances from
  the Sun to the Earth and beyond. The major subsystems of SMEI are an
  electronic Camera Assembly, a Data Handling Unit and interconnection
  harnesses. Each electronic Camera component consists of a baffle,
  radiator, bright object sensor, strongbox (CCD, mirrors and shutter) and
  electronics box. The electronic Camera Assembly is used to observe in
  visible light mass ejections from the Sun by sensing sunlight scattered
  from clouds of solar-produced interplanetary electrons. Predictions
  of arrival time at Earth of this disturbance can be made up to three
  days in advance.

---------------------------------------------------------
Title: Prediction of Solar Wind Conditions in the Inner Heliosphere
    Using IPS Tomography
Authors: Hick, P. P.; Jackson, B. V.; Buffington, A.
2000SPD....31.0241H    Altcode: 2000BAAS...32..818H
  The ability to determine the 3D structure of the co-rotating component
  of the inner heliosphere, and of the 3D extent and evolution of
  solar disturbances superposed on this co-rotating background, are
  of primary importance for effective 'space weather' forecasting. We
  developed a tomographic technique that uses remote sensing data to
  reconstruct a heliospheric solar wind density and velocity model. This
  enables us to reconstruct the background solar wind as well as solar
  disturbances as they move away from the Sun, and forecast their
  subsequent arrival at Earth. Currently we are testing a real-time
  forecasting system based on tomographic reconstructions of the
  solar wind from interplanetary scintillation (IPS) data, available
  on a daily basis from the Solar Terrestrial Environment Laboratory
  (STE-Lab) near Nagoya, Japan. The IPS tomography is used to determine
  velocities at 1 AU where they are compared with in situ observations
  from Earth-orbiting spacecraft. The tomographic solar wind model is
  also used to passively 'convect' Stanford magnetic field data from
  the source outward to 1 AU for comparison with in situ magnetic field
  data. We show current results from this IPS forecasting system. The
  real-time forecasting data are available on a dedicated Web site at
  http://casswww.ucsd.edu/personal/bjackson/weather.htm. This work was
  supported by NSF grant INT-9815377 and AFOSR grant AF49620-97-1-0070.

---------------------------------------------------------
Title: Time-Dependent Tomography Of Heliospheric Features Using
    Global Thomson-Scattering Data From the Helios Spacecraft Photometers
Authors: Jackson, B. V.; Hick, P. P.
2000SPD....3102103J    Altcode: 2000BAAS...32..829J
  In the near future white-light, all-sky imagery of the heliosphere
  will become available from instruments such as the Air Force/NASA Solar
  Mass Ejection Imager (SMEI), and all-sky cameras as currently included
  in the instrument complement of the NASA Solar Probe and Solar Polar
  Sail missions and the ESA Solar Orbiter mission. To optimize the
  information available from these instruments, their 2-dimensional
  sky images need to be interpreted in three dimensions. We have
  developed a Computer Assisted Tomography (CAT) program that modifies
  a time-segmented three-dimensional kinematic heliospheric model to
  fit Thomson scattering observations and is designed specifically with
  observations from the above instrumentation in mind. Here we apply
  this technique to the Helios spacecraft photometer observations. The
  tomography program iteratively changes these models to least-squares
  fit observed global brightness data. The short time intervals of the
  kinematic modeling impose the restriction that the reconstructions
  primarily use outward solar wind motion to give perspective views of
  each point in space accessible to the observations. We plot these
  models as density Carrington maps and remote observer views for
  the Helios data sets. The results to date are commensurate with the
  observational coverage, temporal and spatial resolution, and signal to
  noise available from the original data. At solar maximum, the Helios
  photometer data show significant CME activity in the form of dense
  transient structures at all heliographic latitudes. We explore the
  location of these dense structures with respect to the heliospheric
  current sheet and regions of activity on the solar surface.

---------------------------------------------------------
Title: Commission 10: Solar Activity: (Activite Solaire)
Authors: Ai, G.; Benz, A.; Dere, K. P.; Engvold, O.; Gopalswamy, N.;
   Hammer, R.; Hood, A.; Jackson, B. V.; Kim, I.; Marten, P. C.; Poletto,
   G.; Rozelot, J. P.; Sanchez, A. J.; Shibata, K.; van Driel-Geztelyi, L.
2000IAUTA..24...67A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Three Dimensional Tomography of Heliospheric Features Using
    Global Thomson Scattering Data
Authors: Jackson, B. V.; Hick, P.
2000AdSpR..25.1875J    Altcode:
  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

---------------------------------------------------------
Title: Mercury Sodium Atmosphere, Magnetosphere and Solar Wind
Authors: Killen, R. M.; Giles, B.; Potter, A. E.; Jackson, B. V.;
   Linker, J.; Mikic, Z.
1999DPS....31.1801K    Altcode:
  Earth-based observations of Mercury's sodium atmosphere have revealed
  large-scale spatial variations and rapid temporal variations
  (e.g. Potter and Morgan, Adv. Space Res. 19, 1571, 1997; Potter,
  A.E. et al., Planet. Space. Sci., In press, 1999). We show how
  the observed brightness variations may be related to the topology
  of Mercury's magnetosphere in response to solar wind variations at
  Mercury's orbit. Using the Toffoletto-Hill magnetosphere model modified
  for Mercury (JGR 98, 1339, 1993), we have calculated the structure of
  the Hermean magnetosphere for November, 1997, corresponding to dates
  of our sodium images obtained at the National Solar Observatory at
  Kitt Peak, Arizona. The sodium images are reduced to column abundance
  using a Chamberlain type atmosphere with optically thick radiative
  transfer. Inputs to the magnetosphere model are solar wind density and
  velocity, and interplanetary magnetic field (IMF). Solar wind density
  and velocity at the orbit of Mercury are inferred from heliospheric
  tomography using radio scintillation measurements (Jackson et al.,
  Adv. Space Res. 20, 23, 1997; Kojima et al., JGR 103, 1981, 1998). The
  IMF at Mercury's position is obtained from a model of the inner
  heliosphere constrained with the solar magnetic field, in combination
  with density and temperature profiles at the sun's surface (Linker et
  al., JGR 104, 9809, 1999). We use the morphology of the magnetosphere
  along with solar wind parameters to infer the rates of ion sputtering
  of sodium. The total sodium column is the sum of ion-sputtered sodium
  and the more slowly varying sources, photon-stimulated desorption and
  meteoritic vaporization. We show that the variations in ion sputtering
  and subsequent loss via ioniation may be responsible for rapid changes
  in the observed brightness distribution in sodium emissions. Our goal is
  to show how solar activity and Mercury's sodium exosphere are related.

---------------------------------------------------------
Title: Mercury sodium atmosphere, magnetosphere and solar wind.
Authors: Killen, R. M.; Giles, B.; Potter, A. E.; Jackson, B. V.;
   Linker, J.; Mikic, Z.
1999BAAS...31.1102K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Comparison of solar wind speed with coronagraph data analyzed
    by tomography
Authors: Yokobe, Atsushi; Ohmi, Tomoaki; Hakamada, Kazuyuki; Kojima,
   Masayoshi; Tokumaru, Munetoshi; Jackson, Bernard V.; Hick, Paul P.;
   Zidowitz, Stephan
1999AIPC..471..565Y    Altcode: 1999sowi.conf..565Y
  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<SUB>solar</SUB>)
  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
  1.3-2.0 R<SUB>solar</SUB>. We expect that these provide experimental
  constraints on solar wind acceleration models.

---------------------------------------------------------
Title: Quiet solar wind signatures above active regions observed
    in X-rays
Authors: Hick, P.; Svestka, Z.; Jackson, B. V.; Farnik, F.; Hudson, H.
1999AIPC..471..231H    Altcode: 1999sowi.conf..231H
  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 re-structuring 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.

---------------------------------------------------------
Title: Visible-light All-sky Imagers in Deep Space
Authors: Buffington, A.; Hick, P. P.; Jackson, B. V.
1999AAS...194.7615B    Altcode: 1999BAAS...31..959B
  Emerging new techniques for very wide-angle optics and efficient
  light-baffling systems permit visible-light imagers capable of
  viewing half the sky or more starting within only a few degrees
  of the Sun. These instruments provide the 0.1% photometry required
  for studying low-contrast heliospheric features such as solar mass
  ejections and co-rotating structures. The imagers view sunlight
  Thomson-scattered from interplanetary electrons. A typical imager
  design provides "all-sky" photometric maps with 1 degree sky bins and
  a 1-hour cadence. Instrument weights of only several kilograms and
  modest power requirements make these imagers particularly suitable
  for deployment to deep space. Tomographic reconstructions of the
  interplanetary mass density distribution are enabled by combining
  data from one or more deep-space probes, with comparable instruments
  near Earth. These deep-space images are also suitable for discovery
  and study of comets and asteroids, and for detailed measurements of
  brightness variations in the zodiacal dust cloud.

---------------------------------------------------------
Title: Recent UCSD Advances in Tomography for Use with Heliospheric
    Remote-Sensing Data
Authors: Jackson, B. V.; Hick, P. P.; Buffington, A.
1999AAS...194.7614J    Altcode: 1999BAAS...31R.958J
  Solar disturbances produce major effects in the corona, its
  extension into the interplanetary medium, and ultimately, the Earth's
  environment. The ability to determine the three dimensional extent of
  these disturbances and to forecast their arrival at Earth is of primary
  scientific and practical interest. We have developed a tomographic
  technique for use in mapping these disturbances as they move away from
  the Sun. Our technique uses a solar wind density and velocity model
  and available remote sensing data and iterates to a least squares fit
  solution of these data. This technique provides more contrast between
  high and low speed winds and more or less dense solar wind structures
  than has been possible with previous techniques. Existing observations
  include those from the HELIOS photometers (Thomson scattering data)
  and velocity and scintillation-level measurements (from interplanetary
  scintillation or IPS data). The latter observations are currently
  available on a daily basis from the Solar Terrestrial Environment
  Laboratory situated near Nagoya, Japan. We are developing a way to
  provide a tomographic reconstruction from IPS data in real time for use
  in heliospheric space weather forecasting, and we show our most recent
  results on this. We are also in the process of developing this technique
  to provide the three dimensional extent of heliospheric features which
  vary in shape over short periods of time (i.e., CMEs). The result using
  this extension of the technique is commensurate with the quantity,
  quality and perspective views present from the remote sensing data,
  and with present data is used to explore the extent to which solar
  corotating structures are time-variable. As other remote sensing
  data become available with high angular and temporal resolution
  from spacecraft instruments such as the Solar Mass Ejection Imager
  (SMEI), now being developed and constructed for the Air Force, or as
  proposed for the NASA STEREO or Solar Probe Missions, the technique
  should provide far better heliospheric three dimensional and temporal
  resolution (by several orders of magnitude) than now available.

---------------------------------------------------------
Title: Corrals, hubcaps, and crystal balls: some new designs for
    very-wide-angle visible-light heliospheric imagers
Authors: Buffington, Andrew; Hick, P. P.; Jackson, Bernard V.;
   Korendyke, Clarence M.
1998SPIE.3442...77B    Altcode:
  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 &lt;
  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.

---------------------------------------------------------
Title: Three-dimensional tomography of heliospheric features using
    Thomson scattering data
Authors: Hick, P. P.; Jackson, Bernard V.
1998SPIE.3442...87H    Altcode:
  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 ge put in Earth-orbit will be the solar mass ejection imager,
  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 Probe 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 2D information in
  the all-sky images provided by these cameras to reconstruct the
  heliospheric density structure in 3D. We present preliminary results
  of this tomographic technique applied to Thomson scattering data from
  the photometers onboard the two HELIOS spacecraft.

---------------------------------------------------------
Title: Solar Polar Sail mission: report of a study to put a scientific
    spacecraft in a circular polar orbit about the sun
Authors: Goldstein, Bruce E.; Buffington, Andrew; Cummings, Alan C.;
   Fisher, Richard; Jackson, Bernard V.; Liewer, Paulett C.; Mewaldt,
   Richard A.; Neugebauer, Marcia
1998SPIE.3442...65G    Altcode:
  The Solar Polar Sail Mission uses solar-sail propulsion to place a
  spacecraft in a circular orbit 0.48 Au from the Sun with an inclination
  of 90 degrees. The spacecraft's orbit around the Sun is in 3:1 resonance
  with Earth phased such that the Earth-Sun-spacecraft angle range from 30
  degrees to 150 degrees. The polar view will further our understanding
  of: (1) the global structure and evolution of the corona, (2) the
  initiation, evolution, and propagation of coronal mass ejections; (3)
  the acceleration of the solar wind; (4) the interactions of rotation,
  magnetic fields, and convection within the Sun; (5) the acceleration and
  propagation of energetic particles; and (6) the rate of angular momentum
  loss by the Sun. Candidate imaging instruments are a coronagraph, an
  all-sky imager for following mass ejections and interaction regions
  from the Sun to 1 AU, and a disk imager. A lightweight package of
  fields and particle instruments is included. A mission using a 158 m
  square sail with an effective areal density of 6 g/m(superscript 2)
  would cost approximately $LR 250-300M for all mission phases, including
  the launch vehicle. This mission depends on the successful development
  and demonstration of solar-sail propulsion.

---------------------------------------------------------
Title: Global Solar Wind Changes Over Solar Cycle 21: A Combination
    of HELIOS Photometer, In Situ, and Interplanetary Scintillation Data
Authors: Leinert, Ch.; Jackson, B. V.
1998ApJ...505..984L    Altcode:
  We combine Helios spacecraft photometer brightnesses, in situ plasma
  densities, and interplanetary scintillation (IPS) velocity data to
  obtain a global description of solar wind changes. We find an increase
  of solar mass flux at solar maximum from the photometer brightnesses
  larger than would be expected from the usual assumption of invariant
  momentum flux over solar cycle 21 (1975-1986). A portion of this excess
  mass is related to solar mass ejections, which have an occurrence rate
  that follows the solar activity cycle.

---------------------------------------------------------
Title: Heliospheric tomography using interplanetary scintillation
    observations 1. Combined Nagoya and Cambridge data
Authors: Jackson, B. V.; Hick, P. L.; Kojima, M.; Yokobe, A.
1998JGR...10312049J    Altcode:
  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 N<SUB>e</SUB> for the two data sets with resolutions of
  10° 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 ΔN<SUB>e</SUB>~N<SUB>e</SUB><SUP>0.3</SUP>. 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.

---------------------------------------------------------
Title: Faulting associated with historical and recent earthquakes
    in the Eastern Mediterranean region
Authors: Ambraseys; Jackson
1998GeoJI.133..390A    Altcode:
  This paper summarizes evidence for surface faulting in historical
  and recent earthquakes in the Eastern Mediterranean region and in the
  Middle East. Such information is particularly important for studies
  of active tectonics and for palaeoseismology. We have found 78 cases
  of faulting pre-1900 and 72 post-1900, some of which show that faults
  that have apparently been inactive this century had already ruptured
  before 1900. For some cases faulting could not have been predicted
  from 20th century activity, and in others it could have been expected,
  but has not been observed during the instrumental period. The data are
  sufficient to allow the derivation of relationships between magnitude
  and rupture length.

---------------------------------------------------------
Title: Fan-Like coronal X-ray Structures as Sources of Solar Wind
Authors: Hick, P.; Svestka, Z.; Farnik, F.; Hudson, H. S.; Jackson,
   B. V.
1998AAS...192.1503H    Altcode: 1998BAAS...30..840H
  We show coronal soft X-ray images from the Yohkoh satellite, obtained
  following occurrences of limb flares. These images show rising
  post-flare loops, which are embedded in hot coronal structures looking
  like fans of coronal rays. We analyze the event on 28/29 August 1992,
  which occurred in AR 7270 on the east limb of the Sun. We suggest that
  these rays are multiple 'ministreamers', which apparently are formed as
  a result of the restructuring of the corona following the occurrence
  of a flare-associated CME. We argue that this configuration allows
  outflow of mass from the active region into interplanetary space. This
  is supported by synoptic maps of solar wind sources constructed from
  scintillation measurements showing a source of enhanced scintillation
  at the position of AR 7270.

---------------------------------------------------------
Title: An All-Sky Coronal Camera on Solar Probe: A Global View of
    our Nearest Star's Atmosphere
Authors: Buffington, A.; Jackson, B. V.; Hick, P.
1998AAS...192.1502B    Altcode: 1998BAAS...30..840B
  NASA's proposed Solar Probe mission will provide an opportunity
  to directly view material in the atmosphere of our nearest star:
  the Sun. The Probe is designed to transit both solar poles and
  approach about as close as currently feasible: within about 4
  solar radii. Onboard instruments will directly sample the particle
  composition near the spacecraft and view the solar poles from its
  nearby perspective. UCSD's newly developed lightweight light-baffling
  and very wide-angle optical systems permit viewing Thompson-scattered
  sunlight over nearly the whole sky around the spacecraft to within a
  few degrees of the solar disk. The fly-by's varying perspective will
  enable a 3-dimensional coronal reconstruction having unprecedented
  detail. These observations from within the acceleration region should
  greatly refine our understanding of coronal material propagation.

---------------------------------------------------------
Title: Heliospheric modeling used to map global solar wind flows
Authors: Jackson, B. V.; Hick, P.; Leinert, Ch.; Yokobe, A.
1998AAS...192.1904J    Altcode: 1998BAAS...30..846J
  In a recent paper Leinert and Jackson (1998) analyzed brightness
  observations from the Helios spacecraft photometers, in situ data and
  interplanetary scintillation (IPS) velocities, and used these to model
  global heliospheric plasma changes over solar cycle no. 21. Our analysis
  shows changes in the solar wind flow in terms of mass and velocity
  over one Carrington rotation. We model the available IPS velocity
  observations using a tomographic least squares fit to determine solar
  wind speeds. This technique, crucial to our analysis, provides more
  contrast between high speed winds over the solar poles and low speed
  winds near the equator than possible with previous techniques. Here,
  we confirm the validity of this technique with recent Ulysses spacecraft
  measurements and a comparison between Ulysses-measured solar wind speeds
  and IPS velocities available from the STELab in Japan. The primary
  result of the measurements over solar cycle 21 show the extent to which
  the approximation of constant solar wind momentum flux is valid in more
  detail than was previously possible. Under this assumption we find that
  additional mass at about the 15% level is added to the solar wind at
  solar activity maximum, and that this mass is most likely present in
  the form of discrete events (Coronal Mass Ejections). This implies that
  there are probably two different processes acting to remove solar wind
  from the sun - one provided by a constant coronal energization, and one
  that is associated with the strongest solar magnetic fields. Leinert,
  Ch. and B.V. Jackson, Global Solar Wind Changes Over Solar Cycle 21:
  a Combination of Helios Photometer, In-situ and IPS Data, Astrophys. J.,
  (accepted), 1998.

---------------------------------------------------------
Title: Heliospheric tomography using interplanetary scintillation
    observations 2. Latitude and heliocentric distance dependence of
    solar wind structure at 0.1-1 AU
Authors: Kojima, M.; Tokumaru, M.; Watanabe, H.; Yokobe, A.; Asai,
   K.; Jackson, B. V.; Hick, P. L.
1998JGR...103.1981K    Altcode:
  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 800kms<SUP>-1</SUP> and within
  30° of the solar equator speeds decrease to 400kms<SUP>-1</SUP>
  as observed by Ulysses, and (2) high-speed winds get their final
  speed of 750-900kms<SUP>-1</SUP> within 0.1 AU, and consequently,
  that acceleration of the solar wind is small above 0.1 AU.

---------------------------------------------------------
Title: Heliospheric tomography using interplanetary scintillation
    observations 3. Correlation between speed and electron density
    fluctuations in the solar wind
Authors: Asai, K.; Kojima, M.; Tokumaru, M.; Yokobe, A.; Jackson,
   B. V.; Hick, P. L.; Manoharan, P. K.
1998JGR...103.1991A    Altcode:
  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 δN<SUB>e</SUB> 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
  δN<SUB>e</SUB>~V<SUP>-γ</SUP> with γ=0.5+/-0.15, indicating that
  fractional density fluctuations δN<SUB>e</SUB>/N<SUB>e</SUB> 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., this issue], we
  suggest that the fractional density fluctuation level of the high-speed
  wind evolves with heliocentric distance.

---------------------------------------------------------
Title: Solar Wind Structure at 0.1-1 AU Reconstructed from IPS
    Observations Using Tomography
Authors: Kojima, M.; Asai, K.; Jackson, B. V.; Hick, P. L.; Tokumaru,
   M.; Watanabe, H.; Yokobe, A.
1998asct.conf..207K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Physics of Remotely-Sensed Heliospheric Plasmas
Authors: Jackson, Bernard V.
1997ad...rept.....J    Altcode:
  Solar disturbances produce major effects on the corona, the
  solar wind, the interplanetary medium, and the Earth along with
  its magnetosphere. New techniques have been developed under this
  grant for studying plasma disturbances in the inner heliosphere by
  remotely sensing them. These techniques have used data from the HELIOS
  spacecraft zodiacal light photometers, in situ data and a variety
  of other spacecraft and ground based instruments. The zodiacal light
  photometers on board the two HELIOS spacecraft (data coverage from 1974
  to 1986) provided the first reliable information about the heliospheric
  masses and shapes of propagating disturbances. The investigations
  into the physics of the disturbances sensed by these techniques,
  and the ability to forecast them, have been underway during the
  contract. The data analyses have used YOHKOH spacecraft observations,
  Sacramento Peak Observatory and Mauna Loa (Mark 3) coronagraph data to
  map solar surface features. In addition, interplanetary scintillation
  (IPS) data from the Cambridge, England, Nagoya, Japan, and Ooty,
  India radio telescopes plus ULYSSES and IMP in situ data have been
  used to determine present day conditions in the solar wind.

---------------------------------------------------------
Title: The Physics of Remotely-Sensed Heliospheric Plasmas
Authors: Jackson, Bernard V.
1997ucsd.reptR....J    Altcode:
  Solar disturbances produce major effects on the corona, the
  solar wind, the interplanetary medium, and the Earth along with
  its magnetosphere. New techniques have been developed under this
  grant for studying plasma disturbances in the inner heliosphere by
  remotely sensing them. These techniques have used data from the HELIOS
  spacecraft zodiacal light photometers, in situ data and a variety
  of other spacecraft and ground-based instruments. The zodiacal-light
  photometers on board the two HELIOS spacecraft (data coverage from 1974
  to 1986) provided the first reliable information about the heliospheric
  masses and shapes of propagating disturbances. The investigations into
  the physics of the disturbances sensed by these techniques, and the
  ability to forecast them, have been underway during the contract.

---------------------------------------------------------
Title: Tomography of Heliospheric Structures Using HELIOS Spacecraft
    Photometer Data
Authors: Jackson, B. V.; Hick, P. L.
1997SPD....28.1502J    Altcode: 1997BAAS...29..919J
  We have produced a Computer Assisted Tomography (CAT) program that
  optimizes a three-dimensional heliospheric model to fit observational
  data. We have used this program to reconstruct interplanetary
  scintillation and Helios photometer Thomson-scattering data. The
  program iterates to a least-squares solution fit using solar rotation
  and solar wind outward motion to provide perspective views of each
  point in space accessible to the observations. We plot the optimized
  model as Carrington maps in velocity and density with resolutions
  commensurate with the original data sets. Here we concentrate on the
  Helios photometer Thomson-scattering measurements and explore the
  stability of corotating structures. We map the structures we have
  reconstructed to the solar surface and match these with observations
  from the Sacramento Peak green line coronagraph. We also map these
  structures to the Helios spacecraft where they are compared with data
  measured in situ.

---------------------------------------------------------
Title: Design for the Solar Mass Ejection Imager (SMEI)
Authors: 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.
1997SPD....28.0227K    Altcode: 1997BAAS...29..897K
  The Solar Mass Ejection Imager (SMEI) experiment is designed to detect
  and measure transient plasma features in the heliosphere, including
  coronal mass ejections (CMEs), 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. Data from SMEI will be used to develop models
  and techniques that will, for the first time, allow us to predict the
  onset and magnitude of geomagnetic storms that disrupt space operations
  and affect communications and surveillance activities. We will present
  the current design and observational plans for SMEI. SMEI is currently
  under construction with instrument completion expected in 1999. We
  plan to launch SMEI near the next solar maximum and will make the data
  available to the scientific and space weather forecast communities.

---------------------------------------------------------
Title: Heliospheric Observations of Solar Disturbances and Their
    Potential Role in the Origin of Geomagnetic Storms
Authors: Jackson, Bernard V.
1997GMS....98...59J    Altcode: 1997mast.book...59J
  Ground-based interplanetary scintillation observations began
  heliospheric studies in the early 1960's using remote-sensing
  techniques. These were followed by coronagraph and Helios photometer
  white-light observations, and kilometric radio observations. The
  first solar wind in situ observations were measured by the Mariner
  2 spacecraft three decades ago. These observations show heliospheric
  features which corotate with the Sun, as well as those which only occur
  as single events. For an observer at Earth both types of features can
  manifest themselves as abrupt time variations in the heliospheric
  plasma magnetic field, density, and velocity. On the corotating
  side, recent studies have shown that active regions are associated
  with sustained outflows of plasma at 1 AU in the form of a dense,
  slow-speed solar wind component which can interact with the less
  dense coronal hole regions of the solar wind. Recent work shows that
  the heliospheric manifestations of coronal mass ejections provide a
  significant portion of the solar wind mass (&gt;15%) and energy outflow
  at solar maximum. Both of these types of features have implications in
  terms of their potential for magnetospheric interaction. We are now
  poised to take advantage of several technological advances currently
  underway which will undoubtedly play a key role in complete heliospheric
  plasma characterization in terms of fundamental interplanetary medium
  parameters from the Sun outward.

---------------------------------------------------------
Title: Heliospheric tomography using interplanetary scintillation
    observations
Authors: Jackson, B. V.; Hick, P. L.; Kojima, M.; Yokobe, A.
1997AdSpR..20...23J    Altcode:
  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.

---------------------------------------------------------
Title: Solar wind structure at 0.1-1 AU reconstructed from IPS
    observations using tomography
Authors: Kojima, M.; Asai, K.; Hick, P. L.; Jackson, B. V.; Tokumaru,
   M.; Watanabe, H.; Yokobe, A.
1997AIPC..385...97K    Altcode: 1997recs.conf...97K
  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 750-800 km/s within 0.1
  AU, and subsequently the evolution of solar wind structure is small
  at 0.1-1AU.

---------------------------------------------------------
Title: Solar wind structure analyzed by tomography of interplanetary
    scintillation
Authors: Yokobe, A.; Asai, K.; Hick, P. L.; Jackson, B. V.; Kojima,
   M.; Manoharan, P. K.; Tokumaru, M.; Watanabe, H.
1997IAUJD..19E..59Y    Altcode:
  We have analyzed the global structure of the solar wind in the minimum
  phase of the solar cycle using interplanetary scintillation (IPS)
  observation data obtained at STE Lab. We examined the relation between
  the solar wind velocity V and electron density fluctuations delta
  N<SUB>e</SUB> with CAT analysis, and derived the best fit power-low of
  delta N<SUB>e</SUB> propto V^{- gamma} with gamma = 0.5 plus or minus
  0.15. This result indicates that delta N<SUB>e</SUB>/N in a fast wind
  is lager than that of slow wind. We have then analyzed IPS speed data
  during Carrington rotations 1894--1896, which matched the passage of
  the Ulysses spacecraft of its rapid latitude traversal from southern to
  northern hemisphere. As the result, we confirmed that high-speed regions
  with speed of about 800 km/s are separated from an equatorial low-speed
  region with a sharp velocity gradient at heliographic latitudes of
  15<SUP>circ</SUP> to 20<SUP>circ</SUP> in both hemispheres. This
  latitudinal variation is agreed with Ulysses observations very well.

---------------------------------------------------------
Title: STEREO: a solar terrestrial event observer mission concept
Authors: Socker, Dennis G.; Antiochos, S. K.; Brueckner, Guenter E.;
   Cook, John W.; Dere, Kenneth P.; Howard, Russell A.; Karpen, J. T.;
   Klimchuk, J. A.; Korendyke, Clarence M.; Michels, Donald J.; Moses,
   J. Daniel; Prinz, Dianne K.; Sheely, N. R.; Wu, Shi T.; Buffington,
   Andrew; Jackson, Bernard V.; Labonte, Barry; Lamy, Philippe L.;
   Rosenbauer, H.; Schwenn, Rainer; Burlaga, L.; Davila, Joseph M.; Davis,
   John M.; Goldstein, Barry; Harris, H.; Liewer, Paulett C.; Neugebauer,
   Marcia; Hildner, E.; Pizzo, Victor J.; Moulton, Norman E.; Linker,
   J. A.; Mikic, Z.
1996SPIE.2804...50S    Altcode:
  A STEREO mission concept requiring only a single new spacecraft has been
  proposed. The mission would place the new spacecraft in a heliocentric
  orbit and well off the Sun- Earth line, where it can simultaneously view
  both the solar source of heliospheric disturbances and their propagation
  through the heliosphere all the way to the earth. Joint observations,
  utilizing the new spacecraft and existing solar spacecraft in earth
  orbit or L1 orbit would provide a stereographic data set. The new
  and unique aspect of this mission lies in the vantage point of the
  new spacecraft, which is far enough from Sun-Earth line to allow an
  entirely new way of studying the structure of the solar corona, the
  heliosphere and solar-terrestrial interactions. The mission science
  objectives have been selected to take maximum advantage of this new
  vantage point. They fall into two classes: those possible with the
  new spacecraft alone and those possible with joint measurements using
  the new and existing spacecraft. The instrument complement on the new
  spacecraft supporting the mission science objectives includes a soft
  x-ray imager, a coronagraph and a sun-earth imager. Telemetry rate
  appears to be the main performance determinant. The spacecraft could
  be launched with the new Med-Lite system.

---------------------------------------------------------
Title: Solar Mass Ejection Imager (SMEI)
Authors: Keil, Stephen L.; Altrock, Richard C.; Kahler, Stephen;
   Jackson, Bernard V.; Buffington, Andrew; Hick, Paul; Simnett, George
   M.; Eyles, Christopher J.; Webb, David; Anderson, Peter
1996SPIE.2804...78K    Altcode:
  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) X 3 degree(s) field of view for a total image
  size of 180 degree(s) X 3 degree(s). As the satellite orbits the earth,
  repeated images are used to build up a view of the entire heliosphere.

---------------------------------------------------------
Title: Evidence of active region imprints on the solar wind structure
Authors: Hick, P.; Jackson, B. V.
1996AIPC..382..461H    Altcode:
  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.

---------------------------------------------------------
Title: Coronal synoptic temperature maps derived from the Fe XIV/Fe
    X intensity ratio
Authors: Hick, P.; Jackson, B. V.; Altrock, R. C.
1996AIPC..382..169H    Altcode:
  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 usually 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, temperature maps are available for four heights between
  1.15 and 1.45 R<SUB>solar</SUB>. For these maps the correspondence
  with the current sheet (calculated at 2.5 R<SUB>solar</SUB>) improves
  with height. Discrepancies between temperature structure and magnetic
  structure appear to be largest when the magnetic structure changes
  rapidly from rotation to rotation.

---------------------------------------------------------
Title: Comparison of CME masses and kinetic energies near the sun
    and in the inner heliosphere
Authors: Webb, D. F.; Howard, R. A.; Jackson, B. V.
1996AIPC..382..540W    Altcode:
  Masses have now been determined for many CMEs observed in the inner
  heliosphere by the Helios 1 and 2 zodiacal light photometers. The speed
  of the brightest material of each CME has also been measured so that,
  for events having both mass and speed determinations, their kinetic
  energies can be estimated. We compare the excess masses and kinetic
  energies of individual CMEs estimated in the inner heliosphere by
  Helios and near the Sun from observations by the Solwind (1979-1980)
  and SMM coronagraphs (1980). We also compare the speeds of the same
  CMEs. We find that the Helios mass and energy estimates are larger
  by factors of ~3 and 3-8, respectively, than those derived from the
  coronagraph data. Possible causes for the mass difference include
  the extended flow of CME mass through the corona that is not well
  measured by coronagraphs, and an increase of CME mass with height due
  to compression of ambient solar wind material. These results provide
  an important baseline for observations of CMEs from coronagraphs,
  from the WIND and Ulysses spacecraft and in the near future from SOHO.

---------------------------------------------------------
Title: The solar mass ejection imager
Authors: Jackson, B. V.; Buffington, A.; Hick, P. L.; Kahler, S. W.;
   Altrock, R. C.; Gold, R. E.; Webb, D. F.
1996AIPC..382..536J    Altcode:
  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° 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.

---------------------------------------------------------
Title: The Solar Coronal Temperature Structure and the Heliospheric
    Current Sheet
Authors: Altrock, R. C.; Hick, P.; Jackson, B. V.; Slater, G.; Henry,
   T. W.
1996AAS...188.8004A    Altcode: 1996BAAS...28..956A
  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.

---------------------------------------------------------
Title: Solar coronal structure: a comparison of NSO/SP ground-based
    coronal emission line intensities and temperatures with YOHKOH SXT
    and WSO magnetic data
Authors: Altrock, R. C.; Hick, P.; Jackson, B. V.; Hoeksema, J. T.;
   Zhao, X. P.; Slater, G.; Henry, T. W.
1996AdSpR..17d.235A    Altcode: 1996AdSpR..17..235A
  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 ~ 3 MK), generally occurs only over low-latitude regions
  that are bright in both Fe X (T ~ 1 MK) and Fe XIV (T ~ 2 MK). Thus,
  there is evidence for low (~1 MK), moderate (~2 MK) and high (~3 MK)
  temperatures in close proximity in the low corona.

---------------------------------------------------------
Title: IPS observations of heliospheric density structures associated
    with active regions
Authors: Hick, P.; Jackson, B. V.; Altrock, R.; Woan, G.; Slater, G.
1996AdSpR..17d.311H    Altcode: 1996AdSpR..17..311H
  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
  (≈ 200 km) density variations present in the quiet solar wind.

---------------------------------------------------------
Title: The Coronal Temperature Structure and the Current Sheet
Authors: Hick, Paul; Jackson, B. V.; Altrock, R. C.; Slater, G.;
   Henry, T.
1996ASPC...95..358H    Altcode: 1996sdit.conf..358H
  No abstract at ADS

---------------------------------------------------------
Title: Geomagnetic Storms and Heliospheric CMEs as Viewed From HELIOS
Authors: Webb, David F.; Jackson, Bernard V.; Hick, Paul
1996ASPC...95..167W    Altcode: 1996sdit.conf..167W
  No abstract at ADS

---------------------------------------------------------
Title: The Influence of Active Regions on IPS measurements near 1 AU
Authors: Hick, Paul; Jackson, B. V.
1996ASPC...95..470H    Altcode: 1996sdit.conf..470H
  No abstract at ADS

---------------------------------------------------------
Title: The Solar Mass Ejection Imager (SMEI): Development and Use
    in Space Weather Forecasting
Authors: 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.
1996ASPC...95..158K    Altcode: 1996sdit.conf..158K
  No abstract at ADS

---------------------------------------------------------
Title: Three-dimensional reconstruction of a coronal mass ejection.
Authors: Jackson, B. V.; Froehling, H. R.
1995A&A...299..885J    Altcode:
  We reconstruct the three-dimensional density distribution of a coronal
  mass ejection (CME) in the interplanetary medium from data provided by
  the Helios spacecraft zodiacal light photometers and by the Solwind
  coronagraph. Computer assisted tomography (CAT) techniques can be
  used to reconstruct an image from its projections whenever multiple
  views of optically thin objects are available. In this case Thomson
  scattering of sunlight from electrons is the source of variations
  in observed brightness. Polarization measurements from the Helios
  spacecraft yield additional information about line of sight electron
  densities not normally present in usual CAT-scan techniques. The
  Helios and coronagraph views are not simultaneous; the Helios 16deg
  photometer observes to within 17R<SUB>sun</SUB>_, whereas the Solwind
  observations extend outward to only 10R<SUB>sun</SUB>_. However,
  if we assume radial velocities for ejected material, and that as
  an approximation the velocity of outward-moving material at a given
  height is fixed for the ejection, we obtain a solution. This solution
  is certified by the reconstruction of two test structures - a hollow
  sphere and two spheres of material analyzed by the same techniques
  used to deconvolve the CME. The CAT solution shows that the dense
  structure of the May 7, 1979 CME is distributed in two lobes extending
  over a quarter of a heliospheric hemisphere. We conclude from the CAT
  analysis that the CME material must have accelerated from 100km/s in
  the Solwind field of view to 600km/s in the view from Helios.

---------------------------------------------------------
Title: Evidence of active region imprints on the solar wind structure
Authors: Hick, P.; Jackson, B. V.
1995sowi.conf...48H    Altcode:
  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 possibly neglects important
  aspects of solar wind dynamics

---------------------------------------------------------
Title: The Solar Mass Ejection Imager
Authors: Jackson, B. V.; Buffington, A.; Hick, P. L.; Kahler, S. W.;
   Altrock, R. C.; Gold, R. E.; Webb, D. F.
1995sowi.confR..97J    Altcode:
  We are designing a Solar Mass Ejection Imager (SMEI) capable
  of observing the Thomson-scattered signal from transient density
  features in the heliosphere from a spacecraft situated near 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 these
  observations to the surrounding environment. The observations from
  the instrument should allow deconvolution of these structures from the
  perspective views obtained as they pass the spacecraft. An imager at
  Earth could allow up to three days warning of the arrival of a mass
  ejection from the Sun .

---------------------------------------------------------
Title: Coronal synoptic temperature maps derived from the Fe XIV/Fe
    X intensity ratio
Authors: Hick, P.; Jackson, B. V.; Altrock, R.
1995sowi.confQ..69H    Altcode:
  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 in the range of 1-2 MK. The synoptic
  maps indicate an association between high coronal temperature and the
  large-scale magnetic field. A comparison with WSO '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 temperature maps have been constructed for various heights
  between 1.15 and 1.45 solar radii. For these maps the correspondence
  with the current sheet (calculated at 2.5 solar radii) improves with
  height. Deviations between temperature structure and magnetic structure
  appears to be largest when the magnetic structure changes rapidly from
  rotation to rotation.

---------------------------------------------------------
Title: Comparison of CME masses and kinetic energies near the Sun
    and in the inner heliosphere
Authors: Webb, D. F.; Howard, R. A.; Jackson, B. V.
1995sowi.conf...97W    Altcode:
  Masses have now been determined for many of the CMEs observed in the
  inner heliosphere by the HELIOS 1 and 2 zodiacal light photometers. The
  speed of the brightest material of each CME has also been measured so
  that, for events having both mass and speed determinations, the kinetic
  energies of the CMEs are estimated. We compare the masses and kinetic
  energies of the individual CMEs measured in the inner heliosphere by
  HELIOS and near the Sun from observations by the SOLWIND (1979-1983)
  and SMM coronagraphs (1980). Where feasible we also compare the speeds
  of the same CMEs. We find that the HELIOS masses and energies tend
  to be somewhat larger by factors of 2-5 than those derived from the
  coronagraph data. We also compare the distribution of the masses and
  energies of the HELIOS and coronagraph CMEs over the solar cycle. These
  results provide an important baseline for observations of CMEs from
  coronagraphs, from the ISEE-3/ICE, WIND and Ulysses spacecraft and in
  the future from SOHO.

---------------------------------------------------------
Title: CME masses measured by the HELIOS spacecraft photometers
Authors: Jackson, B. V.; Webb, D. F.
1995sowi.confQ..97J    Altcode:
  We have cataloged 160 CMEs detected in the HELIOS 1 and 2 90 deg
  zodiacal light photometers observed from 1975-1985. The HELIOS 1
  and 2 spacecraft orbited from 0.3 to 1.0 AU on 6-month orbits. From
  the photometer observations of Thomson-scattered light in the inner
  heliosphere, we have determined CME masses for these events using two
  methods: (1) by integration over the contours drawn between the three
  photometers at a given time; and (2) by integration of the mass flow
  over time past a given photometer. The second method, not readily
  available using coronagraph observations, is derived from CME speeds
  measured by using the timing of the peak CME brightness from the 16
  deg to 31 deg sets of photometers. The two different HELIOS methods of
  determining CME mass are consistent with one another for individual
  CMEs. We find that the CME mass values range from 10<SUP>15</SUP>g
  to nearly 10<SUP>17</SUP>g. We compare the mass distributions of
  HELIOS-measured CMEs with those from coronagraphs and find that CMEs
  measured by HELIOS over the same time interval are generally more
  massive. The solar cycle variation of the total CME mass present in
  the heliosphere varies by over a factor of approximately 15 from solar
  minimum to solar maximum. Slightly more massive CMEs carry the bulk
  of the CME mass during maximum. The total CME mass at solar maximum
  is found to be near 15% of the total solar wind mass.

---------------------------------------------------------
Title: Yohkoh/SXT x-ray synoptic maps of coronal brightness and
    temperature
Authors: Slater, G. L.; Lemen, J. R.; Hick, P.; Jackson, B. V.
1995sowi.conf...68S    Altcode:
  The Yohkoh soft X-ray telescope (SXT) records on the order of 50
  solar images per day in two different color filters. These provide
  material for the generation of synoptic maps, which compress the
  3-dimensional data cube into two dimensions. We are creating synoptic
  maps from strips of data both at disk center and at different heights,
  including limb maps that are analogous to those produced by ground-based
  coronagraphs. The ratios of intensities in images taken in two filters
  provide estimates of the electron temperature in the range 1 - 3 x
  10<SUP>6</SUP> K. These are broad-band temperature maps; rather than
  maps created with discrete sampling as in the case of the coronal
  green and red lines. We discuss the properties of these maps and their
  application to the study of energy release in the corona.

---------------------------------------------------------
Title: Synoptic IPS and Yohkoh soft X-ray observations
Authors: Hick, P.; Jackson, B. V.; Rappoport, S.; Woan, G.; Slater,
   G.; Strong, K.; Uchida, Y.
1995GeoRL..22..643H    Altcode:
  Interplanetary scintillation measurements of the disturbance factor,
  g, from October 1991 to October 1992 are used to construct synoptic
  Carrington maps. These maps, which show the structure of the quiet
  solar wind, are compared with X-ray Carrington maps from the Yohkoh
  SXT instrument. For the period studied the global structure outlined
  by (weakly) enhanced g-values apparent in the IPS maps tends to match
  the active regions (as shown in the X-ray maps) significantly better
  than the heliospheric current sheet. Contrary to traditional opinion,
  which views active regions as magnetically closed structures that do
  not have any significant impact on the solar wind flow, our results
  suggest that density fluctuations in the solar wind are significantly
  enhanced over active regions. These results support the suggestion
  by Uchida et al. (1992), based on Yohkoh observations of expanding
  active regions, that active regions play a role in feeding mass into
  the quiet solar wind.

---------------------------------------------------------
Title: Association of Solar Coronal Temperature and Structure from
    Ground-Based Emission-Line Data with Global Magnetic Field Models
    and Yohkoh SXT Data (Abstract only)
Authors: Altrock, R. C.; Hick, P.; Jackson, B. V.; Hoeksema, J. T.;
   Zhao, X. P.; Slater, G.; Henry, T. W.
1995itsa.conf...45A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Coronagraph Stray Light Analyses (Abstract only)
Authors: Jackson, B. V.; Lones, L. A.
1995itsa.conf..199J    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: A spaceborne near-Earth asteroid detection system.
Authors: Jackson, B. V.; Buffington, A.; Hick, P. L.; Kahler, S. W.;
   Webb, D. F.
1994A&AS..108..279J    Altcode:
  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.

---------------------------------------------------------
Title: Three-dimensional reconstruction of coronal mass ejections
Authors: Jackson, B. V.; Hick, P.
1994ESASP.373..199J    Altcode: 1994soho....3..199J
  No abstract at ADS

---------------------------------------------------------
Title: The masses of CMEs measured in the inner heliosphere
Authors: Jackson, B. V.
1994ESASP.373..233J    Altcode: 1994soho....3..233J
  No abstract at ADS

---------------------------------------------------------
Title: Solar wind mass and momentum flux variations at 0.3 AU
Authors: Hick, P.; Jackson, B. V.
1994AdSpR..14d.135H    Altcode: 1994AdSpR..14..135H
  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.

---------------------------------------------------------
Title: Catalog of HELIOS 90 deg photometer events
Authors: Jackson, Bernard V.; Webb, David F.; Hick, Paul L.; Nelson,
   Jessica L.
1994STIN...9436264J    Altcode:
  The two 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 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 degree 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 degree 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.

---------------------------------------------------------
Title: A CME Mass Distribution Derived from SOLWIND Coronagraph
    Observations
Authors: Jackson, Bernard V.; Howard, Russ A.
1993SoPh..148..359J    Altcode:
  Using estimates of the masses of nearly 1000 CMEs observed by SOLWIND
  from Howardet al. (1985), we re-plot the numbers of CMEs as a function
  of CME mass on a log-linear plot. The plot is significant in that
  it shows a linear trend over more than a decade of CME masses. The
  plot indicates a simple form for the distribution of the CME masses
  and allows an easy determination of the total mass ejected into the
  solar wind in the form of CMEs. We find that approximately 16% of
  the solar wind at solar maximum can be comprised of CME mass. There
  is no indication that the numbers of low-mass CMEs increase in number
  above the trend set by the more massive ones. Specifically, there is
  no increase in the numbers of small CMEs such that the whole of the
  solar wind can be comprised of them.

---------------------------------------------------------
Title: Remote sensing of inner heliospheric plasmas
Authors: Jackson, Bernard V.
1993ucsd.rept.....J    Altcode:
  Solar disturbances produce major effects on the corona, the
  solar wind, the interplanetary medium, and the earth along with
  its magnetosphere. We have developed new techniques for studying
  plasma disturbances in the inner heliosphere by remotely sensing
  them. These techniques use data from the HELIOS spacecraft zodiacal
  light photometers and in situ data, the ISEE-3 spacecraft in situ and
  kilometer radio wave experiments, and a variety of other spacecraft
  and ground-based instruments. We use interplanetary scintillation (IPS)
  data from the Cambridge, England, radio telescope. The zodiacal-light
  photometers on board the two HELIOS spacecraft (data coverage from 1974
  to 1986) provide the first reliable information about the heliospheric
  masses and shapes of propagating disturbances.

---------------------------------------------------------
Title: Synoptic Interplanetary Scintillation (IPS) Maps for Use in
    Heliospheric Data Analysis and Space Environment Forecasting
Authors: Rappoport, S. A.; Jackson, B. V.; Hick, P. L.; Davidson,
   T. E.; Winfield, K. A.
1993BAAS...25.1211R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Three Dimensional Reconstruction of Coronal Mass Ejections
Authors: Jackson, B. V.
1993BAAS...25R1211J    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Solar Mass Ejection Imager
Authors: Jackson, B. V.; Buffington, A.; Kahler, S. W.; Webb, D. F.;
   Altrock, R.; Gold, R.
1993BAAS...25.1191J    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book-Review - Physics of the Inner Heliosphere - Part Two -
    Particles Waves and Turbulence
Authors: Schwenn, R.; Marsch, E.; Jackson, B. V.
1993SoPh..145R.405S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book Review: Stellar atmospheres: beyond classical models /
    Kluwer, 1991
Authors: Machado, M. E.; Rompolt, Bogdan; Kleczek, Josip; Jackson,
   B. V.; Machado, M. E.
1993SoPh..145..403M    Altcode: 1993SoPh..145..403C
  No abstract at ADS

---------------------------------------------------------
Title: Observations of Solar Wind 'Halo' Electrons
Authors: Hick, P. L.; Jackson, B. V.; Webb, D. F.
1993BAAS...25.1210H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book-Review - Physics of the Inner Heliosphere - Part One -
    Largescale Phenomena
Authors: Schwenn, R.; Marsch, E.; Jackson, B. V.
1993SoPh..145Q.405S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: A Space-Borne Near-Earth Asteroid Detection System
Authors: Jackson, B. V.; Buffington, A.; Hick, P. L.; Webb, D. F.
1993AAS...182.1503J    Altcode: 1993BAAS...25..815J
  We have designed a Solar Mass Ejection Imager (SMEI) to image transient
  heliospheric features from Earth orbit over the entire sky once every
  90 minutes. The instrument is designed to detect changes in the signals
  from electrons which Thomson-scatter sunlight to a brightness level
  of tenth magnitude per square degree of sky. Here, we explore the
  additional possibility of using such an instrument to detect asteroids
  passing near the Earth. We predict that SMEI will discover about 14
  asteroids per year over ~ 12 m in radius and about 10 meteors in the
  range 0.5 -- 5.0 m in radius.

---------------------------------------------------------
Title: Book-Review - Eruptive Solar Flares
Authors: Svestka, Z.; Jackson, B. V.; Machado, M. E.; Sylwester, J.
1993SSRv...65..186S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Characteristics of CMEs Observed in the Heliosphere Using
    HELIOS Photometer and In-Situ Data
Authors: Webb, D. F.; Jackson, B. V.
1993stp2.conf..381W    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Remote sensing of inner heliospheric plasmas
Authors: Jackson, Bernard V.
1992ucsd.rept.....J    Altcode:
  Solar disturbances produce major effects on the corona, the solar
  wind, the interplanetary medium, and the Earth along with its
  magnetosphere. New techniques for studying plasma disturbances in the
  inner heliosphere by remotely sensing them were developed. These
  techniques use data from the HELIOS spacecraft zodiacal light
  photometers, the ISEE-3 spacecraft kilometer radio-wave experiment,
  and a variety of other spacecraft and ground-based instruments. Use of
  interplanetary scintillation (IPS) data from the Cambridge, England
  radio telescope was added. The zodiacal-light photometers on board
  the two HELIOS spacecraft (data coverage from 1974 to 1986) provide
  the first good information about the heliospheric masses and shapes
  of propagating disturbances. Metric and kilometric type 2 and type 3
  radiation caused by shock waves and fast moving electrons respectively
  are another way to remotely sense the structures which propagate
  outward from the Sun. The best kilometric radio-wave sensing of
  inner heliospheric plasma is available from the ISEE-3 spacecraft,
  and recently these data were used to obtain crude images of the
  Earth's magnetosphere. The investigations into the physics of the
  disturbances sensed by these techniques and the ability to forecast
  them are underway.

---------------------------------------------------------
Title: A model for coronal streamer observations using the SOHO
    coronagraph instrumentation.
Authors: Jackson, Bernard V.
1992ESASP.348...97J    Altcode: 1992cscl.work...97J
  The SOHO coronagraphs will offer an unprecedented opportunity to observe
  coronal streamer material and determine its outward motion. The inner
  C1 and C2 coronagraphs should enable ready indentification of coronal
  streamers and their surface manifestations. The outer C3 coronagraph
  should be able to trace streamers to nearly interplanetary distances
  from the Sun. Using a modeling program designed to determine parameters
  from co-rotating heliospheric material viewed by the Helios spacecraft,
  the author shows the locations in position angle and distance from
  the Sun of several modeled streamers. These models demonstrate the
  expected differences in streamer location when different assumptions
  are used for the outward acceleration of the streamer material.

---------------------------------------------------------
Title: Display Techniques for use in Interplanetary Scintillation
    Analysis and Space Environment Forecasting
Authors: Winfields, K. A.; Rappo Port, S. A.; Jones, L. A.; Jones,
   J.; Jackson, B. V.; Hick, P. L.; Davidson, T. E.
1992AAS...181.8114W    Altcode: 1992BAAS...24.1254W
  No abstract at ADS

---------------------------------------------------------
Title: Solar Mass Ejection Imager: A Precision Photometer for
    Time-Series Measurements of Stars and Solar System Objects
Authors: Buffington, A.; Jackson, B. V.
1992AAS...18110114B    Altcode: 1992BAAS...24.1283B
  No abstract at ADS

---------------------------------------------------------
Title: Study of CMES Observed in the Heliosphere Using HELIOS
    Photometer, Magnetic Field and Plasma Data
Authors: Webb, D. F.; Jackson, B. V.; Reames, D. V.
1992AAS...180.1105W    Altcode: 1992BAAS...24..747W
  The zodiacal light photometers on the two Helios spacecraft have been
  used to identify and study the characteristics of solar mass ejections
  within 1 AU of the Sun. We have compiled a list of all significant
  CMEs detected by the photometers between 1975 and 1985. We examine
  the in-situ characteristics of a subset of these CMEs which enveloped
  the spacecraft. In particular, we present results of analyses of
  structures considered to be manifestations of interplanetary CMEs,
  such as magnetic "clouds", shocks and periods of bidirectionally
  streaming ions at energies of about 1 MeV. An important advantage of
  this data set is that it permits us to make reliable associations in
  the interplanetary medium over a long time base between many white
  light CMEs and their in-situ proxies.

---------------------------------------------------------
Title: Remote Sensing Observations of Mass Ejections and Shocks in
    Interplanetary Space
Authors: Jackson, B. V.
1992LNP...399..248J    Altcode: 1992esf..coll..248J; 1992IAUCo.133..248J
  It has long been known that disturbances can propagate from Sun to
  Earth with periods of a few days following large solar flares. These
  disturbances involve a significant portion of the lower solar corona and
  the energy of the flare. Several techniques have been used to remotely
  detect and follow different structures as they propagate outward from
  the Sun. These techniques include interplanetary scintillation (IPS),
  kilometric radio and HELIOS photometer observations. Structures in the
  interplanetary medium can generally be classed as those which propagate
  outward from the Sun and those which co-rotate with approximately the
  solar rotation rate. In this review I will concentrate on ejecta and
  shocks known to be associated with large solar flares observed on the
  surface of the Sun and their manifestations using various observational
  techniques. The observational techniques most commonly used are each
  sensitive to a specific type of structure and more sensitive at one
  portion of the interplanetary medium than another. Because of the
  different techniques used, there can often be misinterpretation of the
  data. In addition, none of the remote sensing observations has complete
  spatial or temporal coverage. Thus, both the basic physics as well as
  the spatial and temporal evolution of mass ejections can be confused
  as these events propagate through the interplanetary medium. Examples
  of the data related to mass ejections from each of these techniques
  are shown and interpreted. We expect that future observations will
  more accurately describe the structures present as their basic physics
  becomes better known.

---------------------------------------------------------
Title: Solar-generated disturbances in the heliosphere
Authors: Jackson, B. V.
1992sws..coll..623J    Altcode:
  It has long been known that disturbances can propagate from Sun to
  Earth with periods of a few days following large solar flares. Other
  disturbances re-occur with the solar rotation rate implying that they
  are more or less stably generated by a specific region on the solar
  surface. At the Sun some of these disturbances are readily observed
  in coronagraphs and against the solar disk. Several techniques have
  been used to remotely detect and follow different disturbances in the
  interplanetary medium as they propagate outward from the Sun. These
  techniques include interplanetary scintillation, kilometric radio
  and Helios photometer observations. In situ, spacecraft can mark
  the passage of disturbances by direct measurement along the column
  convected past the observation point. As probes of the heliospheric
  magnetic field and disturbances in themselves, particles above the
  energy of the thermal plasma traverse the heliosphere and indicate
  the extent of its structures. Both the basic physics, as well as
  the spatial and temporal evolution of disturbances, can be confused
  as they propagate through the interplanetary medium largely because
  of the data coverage limitations. However, as their basic physics
  becomes better known through more complete observations and theory,
  the extent and accuracy of these disturbances can be better described.

---------------------------------------------------------
Title: Considerations of a Solar Mass Ejection Imager in a Low
    Earth Orbit
Authors: Jackson, B. V.; Webb, D. F.; Altrock, R. C.; Gold, R.
1992LNP...399..322J    Altcode: 1992esf..coll..322J; 1992IAUCo.133..322J
  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° 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.

---------------------------------------------------------
Title: Eruptive Solar Flares
Authors: Svestka, Zdenek; Jackson, Bernard V.; Machado, Marcos E.
1992LNP...399.....S    Altcode: 1992IAUCo.133.....S; 1992esf..coll.....S
  This is an exhaustive survey of present-day solar research including
  both theory and observations. It deals with eruptive flares, filament
  eruption in x-rays and radio waves, energy release and transport, and
  terrestrial response to solar flares. Details of the most recent SOLAR-A
  project (launched shortly after the conference) are also presented.

---------------------------------------------------------
Title: Characteristics of CMEs observed in the heliosphere using
    HELIOS photometer data
Authors: Webb, D. F.; Jackson, B. V.
1992sws..coll..681W    Altcode:
  The zodiacal light photometers on the two Helios spacecraft have been
  used to detect and study mass ejections and other phenomena emanating
  from the sun and traversing the heliosphere within 1 AU. We have
  recently compiled a complete list of all of the significant white light
  transient events detected from the 90-deg photometers on both Helios
  spacecraft. This is a preliminary report on the long-term frequency
  of occurrence of these events; it emphasizes newly processed data from
  Helios-l from 1975 through 1982 and viewed south of the ecliptic. With
  the large Helios photometer data base, we will be able to identify
  the fraction of the 90 deg events which are heliospheric CMEs and
  determine their characteristics.

---------------------------------------------------------
Title: Synoptic maps of heliospheric Thomson scattering brightness
    from 1974-1985 as observed by the HELIOS photometers
Authors: Hick, P.; Jackson, B. V.; Schwenn, R.
1992sws..coll..187H    Altcode:
  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 photometer
  coverage is most complete. Because the technique has been used on the
  complete Helios data set from 1974 to 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.

---------------------------------------------------------
Title: Electron Groups Traced from the Sun to 1-AU
Authors: Jackson, Bernard V.; Leblanc, Yolande
1991SoPh..136..361J    Altcode:
  We trace electrons from the Sun by a variety of proxy methods - solar
  flare positions, and metric and kilometric type III radio bursts from
  the Sun until they can be observed in situ as electrons at the ISEE-3
  spacecraft. Our study extends over the period of operation of the
  electron experiment on ISEE-3 from August 1978 to November 1979. By
  carefully restricting timing within the data sets involved, we find a
  peak in the number of flares associated with in situ electrons near 60°
  west solar longitude. This peak shows that type III bursts can be fairly
  limited in spatial extent, and that the best connection with the solar
  surface to the flare is along the Archimedean magnetic field spiral. We
  use this spatial determination to define an `average' beam shape for
  an event. We assume this average beam shape to be representative of the
  distribution in space of each electron group. The electron numbers at 2
  and 29-45 keV energies combined with this average beam shape are used
  to approximate the total numbers of electrons and energy per burst
  for individual events. We find that the total number of electrons
  and total energy for events varies significantly with flare type;
  that on the average brighter flares are associated with more electrons.

---------------------------------------------------------
Title: Remote sensing of inner heliospheric plasmas
Authors: Jackson, Bernard V.
1991ucsd.rept.....J    Altcode:
  Solar disturbances produce major effects on the corona, the solar
  wind, the interplanetary medium, and the Earth along with its
  magnetosphere. We have developed new techniques for studying plasma
  disturbances in the inner heliosphere by remotely sensing them. These
  techniques use data from the HELIOS spacecraft zodiacal light
  photometers, the ISEE-3 spacecraft kilometer radio-wave experiment,
  and a variety of other spacecraft and ground-based instruments. The
  zodiacal light photometers on board the two HELIOS spacecraft (data
  coverage from 1974 to 1986) provide the first good information about
  the heliospheric masses and shapes of propagating disturbances. Metric
  and kilometric type II and type III radiation caused by shock waves
  and fast moving electrons respectively are another way to remotely
  sense the structures which propagate outward from the Sun. The best
  kilometric radio wave sensing of inner heliospheric plasma is available
  from the ISEE-3 spacecraft. The investigations into the physics of the
  disturbances sensed by these techniques and the ability to forecast
  their occurrences are well underway.

---------------------------------------------------------
Title: Helios spacecraft photometer observation of elongated
    corotating structures in the interplanetary medium
Authors: Jackson, B. V.
1991JGR....9611307J    Altcode:
  The Helios spacecraft zodiacal light photometers can be used to
  measure persistent elongated structures at interplanetary distances
  from the Sun. These data give the heliospheric poistions of these
  structures from their east to west motion with time. An outward motion
  of the material within each structure can be determined from its
  curvature. This technique has been used to measure over 40 of these
  structures from solar minimum to solar maximum (1976 through 1979)
  using both Helios A and Helios B observations. The positions of the
  structures measured range from low latitude to as high as 50°. The
  speeds determined have a mean value of 301+/-47 km s<SUP>-1</SUP>. The
  modeling, which determines densities for these structures from 0.15
  to over 1.0 AU, indicates that these heliospheric structures can have
  densities many times above the ambient and that the density in excess
  of an r<SUP>-2</SUP> ambient can differ greatly along their curved
  extents at any given time. Most of the structures measured in this
  sample either remain approximately the same density or decrease in
  density with height above the Sun. This implies that these structure
  are generally remnants of features maintained by the physical processes
  which formed them near the surface of the Sun (as streamers) and that
  they are not caused by interplanetary interactions.

---------------------------------------------------------
Title: Synoptic maps for the heliospheric Thomson scattering
    brightness as observed by the HELIOS photometers
Authors: Hick, P.; Jackson, B. V.; Schwenn, R.
1991A&A...244..242H    Altcode:
  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 is presented. 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
  examples 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. It is expected
  that the Helios synoptic maps will be particularly useful in the study
  of corotating structures (e.g., streamers), and the maps will be most
  reliable during periods when few transient featurs are present in the
  corona, i.e., during solar minimum.

---------------------------------------------------------
Title: The identification and characteristics of solar mass ejections
    observed in the heliosphere by the HELIOS 2 photometers
Authors: Webb, D. F.; Jackson, B. V.
1990JGR....9520641W    Altcode:
  Observations were obtained using the three zodiacal light photometers
  of the Helios 2 spacecraft in order to identify coronal mass ejections
  (CMEs) in the interplanetary medium, to establish their heliospheric
  characteristics, to compare them with those of CMEs observed near
  the sun, and to determine the frequency of occurrence of CMEs from
  1976 through 1979. Eighty percent of the white light transients are
  be classified as CMEs moving outward from the sun. The average CME
  is found to have a brightness increase of 2.3 S10 units in the 90-deg
  photometer, an average duration of 37 h, and a speed of about 500 km/s,
  implying a radial 'flow' dimension of about 0.4 AU, and a longitudinal
  width near the sun of about 50 deg. The CMEs supply significant amounts
  of mass to the inner heliosphere, especially around the maximum phase
  of solar activity. During the rise of the last solar activity cycle,
  the CME occurrence rate increased by an order of magnitude between
  cycle minimum and maximum.

---------------------------------------------------------
Title: On Representing the Large-scale Structure of the Inner
    Heliosphere in Synoptic Maps
Authors: Hick, P.; Jackson, B. V.; Schwenn, R.
1990BAAS...22..810H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Helios Spacecraft Zodiacal Light Photometers Used for
    Comet Observations and Views of the Comet West Bow Shock
Authors: Jackson, B. V.; Benensohn, R. M.
1990EM&P...48..139J    Altcode:
  The HELIOS A and B zodiacal light photometers can be used to view
  comets as they pass the spacecraft. Because the HELIOS spacecraft
  orbit the Sun on their own, and are generally far from Earth, the
  spacecraft allow us to view comets from a different perspective than
  normally available. Comet West (1976VI) passed through perihelion on
  February 25, 1976. The comet crossed the HELIOS A and B spacecraft
  zodiacal light photometer fields of view, allowing them to record the
  brightness, polarization and color of the comet. Data from the U,
  B and V photometers showed a distinct blueing followed by a slight
  reddening corresponding to the ion and dust tails, respectively,
  entering the field of view of each photometer sector. The extent of
  the tail of Comet West was far greater seen from the HELIOS spacecraft
  than seen from Earth, even taking into account their generally closer
  viewing perspective. As Comet West traveled away from the Sun, it was
  observed in the zodiacal light photometer fields of view at a solar
  distance of more than 1.4 AU. The zodiacal light photometers also
  viewed Comet Meier (1978XXI). Comet Meier is far more compact than
  Comet West, extremely blue and unlike Comet West showed no significant
  dust tail. The interplanetary medium is observed to a level of the
  variations in the brightness of the electron-scattering component near
  Comet West. A brightness “bump” present in the data before the
  comet reached some photometer positions can be shown to approximately
  form a parabolic shape sunward and ahead of the orbital motion of
  the Comet West nucleus. We presume that this bump is evidence of the
  position of the cometary atmosphere or an enhancement of the ambient
  interplanetary medium ahead of the comet motion. The brightness bump
  in terms of density generally corresponds to a density enhancement of
  the ambient medium by a few times in the vicinity of the comet. When
  compared with Comet Halley and couched in terms of the shock stand-off
  distance, the distance of this brightness increase from the nucleus
  implies a neutral gas production rate of approximately 2.5 times that
  of Halley. This is in agreement with the neutral gas production rate
  measured from Comet West using more direct techniques.

---------------------------------------------------------
Title: Type-Iii Bursts Traced from the Solar Surface to 1-AU
Authors: Leblanc, Yolande; Jackson, Bernard V.
1990IAUS..142..509L    Altcode:
  Type III radio bursts were traced from the sun until they can be
  observed as in situ electrons at the ISEE-3 spacecraft. The study
  extends over the period of operation of the electron experiment on
  ISEE-3 from August 1978 to November 1979. The observations include data
  from solar flares, kilometric-type III burst spectra from ISEE-3, and
  in situ measurements of low-energy electrons from ISEE-3. By carefully
  restricting the data sets involved, a peak is found of 20-deg width
  in the number of flares associated with in situ electrons near 60-deg
  west solar longitude. This peak shows that the electron beams of type
  III bursts are not spread over a great range of longitudes as earlier
  studies indicate, but are fairly limited in spatial extent. However,
  even in that longitude range, only 40 percent of type-III-flare events
  are associated with in situ electrons.

---------------------------------------------------------
Title: Broad-Band Images of Akr from ISEE-3
Authors: Jackson, Bernard V.; Steinberg, Jean-Louis
1990LNP...362..102J    Altcode: 1990lfas.work..102J
  The ISEE-3 observations (Steinberg et al., 1989) showed that radio
  waves from naturally-occurring auroral kilometric radiation (AKR)
  in the range of 45 to 150 kHz can, in some instances, be refracted
  or ducted away from the location of the radio source. Linear contour
  images of AKR source intensity at different frequencies, observed on
  three different days when the solar wind density had different values
  are presented as an evidence of this, showing that, as seen from ISEE-3,
  the apparent location of the radiation from the spacecraft can be many
  degrees tailward of the earth.

---------------------------------------------------------
Title: Type III Electron Beamwidth from Solar Flare Longitudinal
    Distributions.
Authors: Jackson, B. V.
1990ppsa.conf..209J    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Interplanetary Solar Wind Brightness Synoptic Maps from the
    HELIOS Zodiacal Light Photometers
Authors: Hick, P. L.; Jackson, B. V.; Schwenn, R.
1989BAAS...21..858H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Remote Observation of Co-rotating Interplanetary Structures
    Using the HELIOS Zodiacal Light Photometers
Authors: Jackson, B. V.
1989BAAS...21..858J    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Giant solar arches and coronal mass ejections in November 1980
Authors: Svestka, Zdenek F.; Jackson, Bernard V.; Howard, Russell A.;
   Sheeley, Neil R., Jr.
1989SoPh..122..131S    Altcode:
  Using data from the SOLWIND coronagraph and photometers aboard
  HELIOS-A we examine coronal mass ejections from an active region
  which produced a series of giant post-flare coronal arches. HXIS
  X-ray observations reveal that in several cases underlying flares
  did not disrupt these arch structures, but simply revived them,
  enhancing their temperature, density and brightness. Thus we are
  curious to know how these quasi-stationary X-ray structures could
  survive in the corona in spite of recurrent appearances of powerful
  dynamic flares below them. We have found reliable evidence that two
  dynamic flares which clearly revived the preexisting giant arch were
  not associated with any mass ejection. After two other flares, which
  were associated with mass ejections, the arch might have been newly
  formed when the ejection was over. In one of these cases, however,
  the arch had typical characteristics of a revived structure so that
  it is likely that it survived a powerful mass ejection nearby. In a
  magnetic configuration of the arch which results from potential-field
  modelling (Figure 1(b)) such a survival seems possible.

---------------------------------------------------------
Title: Design considerations for a "Solar Mass Ejection Imager"
    on a rotating spacecraft.
Authors: Jackson, B. V.; Hudson, H. S.; Nichols, J. D.; Gold, R. E.
1989GMS....54..291J    Altcode: 1989opss.conf..291J; 1989sspp.conf..291J
  The authors describe an instrument capable of imaging the time-varying
  features of the entire outer corona (from near the Sun to beyond
  90° elongation) via the Thomson-scattered diffuse solar light. This
  "all sky" imager works on a spin-stabilized spacecraft, preferably in
  deep space.

---------------------------------------------------------
Title: Three-dimensional reconstruction of coronal mass ejections
Authors: Jackson, B. V.
1989AdSpR...9d..69J    Altcode: 1989AdSpR...9...69J
  We use computer assisted tomography (CAT) techniques to reconstruct the
  three-dimensional shapes of coronal mass ejections in the interplanetary
  medium. Thomson scattering of sunlight from electrons is assumed to
  be the source of variations in observed brightness in data provided
  by the HELIOS spacecraft zodiacal light photometers and by the
  SOLWIND coronagraph. Polarization measurements from the spacecraft
  yield additional information about line-of-sight electron densities
  not normally present in usual CAT-scan techniques. Here we use the
  technique to determine the density of a mass ejection which arose
  from the Sun on 7 May 1979. The HELIOS and coronagraph perspective
  views are not simultaneous; the HELIOS 16° photometer observes to
  as close a height as 17R<SUB>solar</SUB> from the Sun, whereas the
  SOLWIND observations extend outward to sky plane distances of only
  10R<SUB>solar</SUB>. However, if radial velocities for the ejected
  material are assumed, and that, as an approximation, the velocity of
  outward-moving material at a given height is everwhere the same, we
  obtain a solution. The least-squares solution provides the velocity
  of the material with height as well as a three-dimensional density
  distribution. The material of the mass ejection appears to accelerate
  at solar distances as great as 10R<SUB>solar</SUB>.

---------------------------------------------------------
Title: Coronal mass ejections and coronal structures.
Authors: Hildner, E.; Bassi, J.; Bougeret, J. L.; Duncan, R. A.;
   Gary, D. E.; Gergely, T. E.; Harrison, R. A.; Howard, R. A.; Illing,
   R. M. E.; Jackson, B. V.; Kahler, S. W.; Kopp, K.; Low, B. C.; Lantos,
   P.; Phillips, K. J. H.; Poletto, G.; Sheeley, N. R., Jr.; Stewart,
   R. T.; Svestka, Z.; Waggett, P. W.; Wu, S. T.
1989epos.conf..493H    Altcode:
  The work of this team was concerned with modelling of post-flare arches,
  the reconnection theory of flares, the slow variation of coronal
  structure, and the coronal and interplanetary detection, evolution,
  and consequences of mass ejections.

---------------------------------------------------------
Title: Heliospheric remote sensing using the zodiacal light
    photometers of the Helios spacecraft.
Authors: Jackson, B. V.
1989GMS....54..287J    Altcode: 1989sspp.conf..287J; 1989opss.conf..287J
  The Helios spacecraft zodiacal light photometers have been used to image
  solar mass ejections, corotating heliospheric density enhancements and
  density enhancements behind shock waves to distances of 1 AU from the
  Sun. To first order, sunlight scattered from heliospheric electrons
  provides the measured brightness ascribed to these features. Remote
  sensing observations of these features indicate extensive structures
  which propagate throughout the inner heliosphere.

---------------------------------------------------------
Title: Solar and interplanetary observations of the mass ejection
    on 7 May, 1979
Authors: Jackson, Bernard V.; Rompolt, Bogdan; Svestka, Zdenek
1988SoPh..115..327J    Altcode:
  We present observations of a mass ejection that was observed by five
  different instruments along its way from the solar surface to more
  than 100 solar radii. The instruments involved are the ground-based
  Hα coronagraph at Wrocław, the white-light SOLWIND coronagraph on
  board the P78-1 satellite, zodiacal light photometers of the HELIOS
  B spacecraft, in situ plasma detectors and magnetometers on board the
  HELIOS B spacecraft, and interplanetary scintillation measurements on
  the ground. By using a CAT-scan analysis of the images obtained by the
  SOLWIND coronagraph near the Earth and HELIOS B photometers placed at
  0.3 AU perpendicular to the Earth-Sun line, we have been able to get a
  three-dimensional density reconstruction of the mass ejection and fit
  the best velocity curve for its propagation. Although problems exist
  in smoothly joining the height-time curves (for instance, we had to
  reduce the brightness of the SOLWIND data by more than a factor of two
  to make the data sets agree photometrically), both this analysis and
  direct measurements by the other experiments clearly indicate higher
  speeds at greater distances from the Sun. The plasma acceleration
  in this case was obviously not limited only to distances within 3
  R<SUB>0</SUB>, as is usually the case, but continued beyond the outer
  limit of the coronagraph view at ∼ 8 R<SUB>0</SUB>.

---------------------------------------------------------
Title: Scientific background and design specifications for a
    near-earth heliospheric imager
Authors: Jackson, B. V.
1988ucsd.rept.....J    Altcode:
  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 it is possible to
  determine the velocities 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.

---------------------------------------------------------
Title: Comet West: A view from the HELIOS zodiacal light photometers
Authors: Benensohn, R. M.; Jackson, B. V.
1987sici.symp...46B    Altcode:
  Comet West passed through perihelion on February 25, 1976. The comet
  crossed the HELIOS A and B spacecraft zodiacal light photometer fields
  of view as the spacecraft orbited the Sun, allowing them to record the
  brightness, polarization, and color of the comet and its surrounding
  interplanetary medium. Data from the U, B, and V photometers across
  the tail shows a distinct bluing followed by a slight reddening
  corresponding to the ion and dust tails, respectively, entering the
  field of view. The non-Earth perspective of the HELIOS photometers
  allows a comparison of the tail with Earth observations at the same
  time. Precise location of the nucleus and tail allow the photometer
  data to be searched for evidence of the comet bow shock and orbital
  dust. A brightness bump present in the data before the comet reaches
  some photometer positions, can be shown to approximately form a
  parabolic shape Sunward and ahead of the orbital motion of the Comet
  West nucleus. If this is the comet bow shock or bow compression, then
  it corresponds to a density enhancement of the ambient medium by 1.5 to
  2 times in the vicinity of the comet. The distance of the brightness
  increase from the nucleus by comparison with Comet Halley implies a
  neutral gas production rate of approximately 3 times that of Halley.

---------------------------------------------------------
Title: Three-Dimensional Reconstruction of Coronal Mass Eiections
Authors: Froehling, B. R.; Jackson, B. V.
1987BAAS...19R.931F    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: A Current System Asymmetry Relative to the Poles of an
    Expanding Bipolar Active Region
Authors: Jackson, B. V.
1987BAAS...19..941J    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar and Interplanetary Observations of the Mass Ejection
    on 7 May 1979
Authors: Jackson, B. V.; Rompolt, B.; Svestka, Z.
1987sowi.conf..272J    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Detection of CMEs in the Interplanetary Medium from 1976-1979
    Using Helios-2 Photometer data
Authors: Webb, D. F.; Jackson, B. V.
1987sowi.conf..267W    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Interplanetary Effects of Coronal Mass Ejections
Authors: Hildner, E.; Bassi, J.; Bougeret, J. L.; Duncan, R. A.;
   Gary, D. E.; Gergely, T. E.; Harrison, R. A.; Howard, R. A.; Illing,
   R. M. E.; Jackson, B. V.; Kahler, S. W.; Kopp, K.; Low, B. C.; Lantos,
   P.; Phillips, K. J. H.; Poletto, G.; Sheeley, N. R., Jr.; Steward,
   R. T.; Svestka, Z.; Waggett, P. W.; Wu, S. T.
1986epos.conf.6.52H    Altcode: 1986epos.confF..52H
  No abstract at ADS

---------------------------------------------------------
Title: Initiations of Coronal Mass Ejections
Authors: Hildner, E.; Bassi, J.; Bougeret, J. L.; Duncan, R. A.;
   Gary, D. E.; Gergely, T. E.; Harrison, R. A.; Howard, R. A.; Illing,
   R. M. E.; Jackson, B. V.; Kahler, S. W.; Kopp, K.; Low, B. C.; Lantos,
   P.; Phillips, K. J. H.; Poletto, G.; Sheeley, N. R., Jr.; Steward,
   R. T.; Svestka, Z.; Waggett, P. W.; Wu, S. T.
1986epos.conf.6.27H    Altcode: 1986epos.confF..27H
  No abstract at ADS

---------------------------------------------------------
Title: The Slowly Varying Corona Near Solar Activity Maximum
Authors: Hildner, E.; Bassi, J.; Bougeret, J. L.; Duncan, R. A.;
   Gary, D. E.; Gergely, T. E.; Harrison, R. A.; Howard, R. A.; Illing,
   R. M. E.; Jackson, B. V.; Kahler, S. W.; Kopp, K.; Low, B. C.; Lantos,
   P.; Phillips, K. J. H.; Poletto, G.; Sheeley, N. R., Jr.; Steward,
   R. T.; Svestka, Z.; Waggett, P. W.; Wu, S. T.
1986epos.conf.6.57H    Altcode: 1986epos.confF..57H
  No abstract at ADS

---------------------------------------------------------
Title: Modelling of Coronal Mass Ejections and POST Flare Arches
Authors: Hildner, E.; Bassi, J.; Bougeret, J. L.; Duncan, R. A.;
   Gary, D. E.; Gergely, T. E.; Harrison, R. A.; Howard, R. A.; Illing,
   R. M. E.; Jackson, B. V.; Kahler, S. W.; Kopp, K.; Low, B. C.; Lantos,
   P.; Phillips, K. J. H.; Poletto, G.; Sheeley, N. R., Jr.; Steward,
   R. T.; Svestka, Z.; Waggett, P. W.; Wu, S. T.
1986epos.conf6.366H    Altcode: 1986epos.confF.366H
  No abstract at ADS

---------------------------------------------------------
Title: Coronal mass ejections and coronal structures
Authors: Hildner, E.; Bassi, J.; Bougeret, J. L.; Duncan, R. A.;
   Gary, D. E.; Gergely, T. E.; Harrison, R. A.; Howard, R. A.; Illing,
   R. M. E.; Jackson, B. V.
1986epos.conf..6.1H    Altcode: 1986epos.confF...1H
  Research on coronal mass ejections (CMF) took a variety of forms, both
  observational and theoretical. On the observational side there were:
  case studies of individual events, in which it was attempted to provide
  the most complete descriptions possible, using correlative observations
  in diverse wavelengths; statistical studies of the properties CMEs and
  their associated activity; observations which may tell us about the
  initiation of mass ejections; interplanetary observations of associated
  shocks and energetic particles even observations of CMEs traversing
  interplanetary space; and the beautiful synoptic charts which show to
  what degree mass ejections affect the background corona and how rapidly
  (if at all) the corona recovers its pre-disturbance form. These efforts
  are described in capsule form with an emphasis on presenting pictures,
  graphs, and tables so that the reader can form a personal appreciation
  of the work and its results.

---------------------------------------------------------
Title: A Metric Type-Iii Burst Asymmetry Relative to Simple Bipolar
    Active Regions
Authors: Jackson, B. V.
1986SoPh..105..123J    Altcode:
  Metric type III solar radio burst positions are compared spatially
  and temporally to underlying active region geometry. The positions of
  these radio bursts have an asymmetric location distribution relative
  to simple bipolar regions. The type III bursts show a tendency to
  occur nearer the leading active region - an association shown before
  from type III burst and magnetic field polarity measurements. The type
  III bursts also generally occur to the left of the outward to inward
  directed magnetic field. The asymmetry relative to the outward directed
  magnetic field has a sense that is consistent with a mechanism of
  type III burst production that involves a pre-existing coronal current
  system situated between expanding closed and open magnetic field lines.

---------------------------------------------------------
Title: Coronal mass ejection associated with the stationary post-flare
    arch of 21 22 May 1980
Authors: McCabe, Marie K.; Švestka, Zdeněk F.; Howard, Russell A.;
   Jackson, Bernard V.; Sheeley, Neil R.
1986SoPh..103..399M    Altcode:
  By using a combination of X-ray (HXIS), Hα (Haleakala), white-light
  corona (Solwind), and zodiacal light (Helios) images on 21-22 May, 1980
  we demonstrate, and try to explain, the co-existence of a coronal mass
  ejection with a stationary post-flare coronal arch. The mass ejection
  was seen, both by Solwind and Helios, in prolongation of the path of
  a powerful spray, whereas the active region filament did not erupt. A
  tentative comparison is made with other occurrences of stationary,
  or quasi-stationary post-flare coronal arches.

---------------------------------------------------------
Title: Coronal mass ejections and coronal structures.
Authors: Hildner, E.; Bassi, J.; Bougeret, J. L.; Duncan, R. A.;
   Gary, D. E.; Gergely, T. E.; Harrison, R. A.; Howard, R. A.; Illing,
   R. M. E.; Jackson, B. V.; Kahler, S. W.; Kopp, K.; Low, B. C.; Lantos,
   P.; Phillips, K. J. H.; Poletto, G.; Sheeley, N. R., Jr.; Stewart,
   R. T.; Svestka, Z.; Waggett, P. W.; Wu, S. T.
1986NASCP2439....6H    Altcode:
  Contents: 1. Introduction. 2. Observations. 3. Initiation of
  coronal mass ejections - observations. 4. Modelling of coronal mass
  ejections and post-flare arches. 5. Interplanetary effects of coronal
  mass ejections. 6. The slowly varying corona near solar activity
  maximum. 7. Summary.

---------------------------------------------------------
Title: HELIOS photometer measurements of in-situ density enhancements
Authors: Jackson, B. V.
1986AdSpR...6f.307J    Altcode: 1986AdSpR...6..307J
  The HELIOS spacecraft zodiacal light photometers have been used to image
  coronal mass ejections and coronal streamers in the interplanetary
  medium. The HELIOS photometers have the ability to image such
  features beyond 90° angular distance from the Sun. This provides
  a unique opportunity to measure brightness enhancements which are
  also observed as density increases in situ by the HELIOS spacecraft
  plasma probes. Here, I compare the brightness enhancements and in situ
  density increases following shocks defined by the plasma and magnetic
  field data. Five well-observed shocks from 1976 and 1979 illustrate
  these comparisons. Each event can be followed in photometer data as it
  sweeps past the HELIOS spacecraft. To first order, the enhancements
  of brightness following shocks indicate structures which extend over
  many tenths of an astronomical unit and colors which are consistent
  with Thomson scattering of sunlight by electrons.

---------------------------------------------------------
Title: Helios Images of Coronal Mass Ejections
Authors: Jackson, B. V.
1986shtd.symp..113J    Altcode:
  The zodiacal light photometers on board the HELIOS spacecraft can be
  used to form images of coronal mass ejections in the interplanetary
  medium. Several aspects of these data are unique: they trace coronal
  mass ejections using Thomson scattering techniques to distances from
  the Sun greater than 0.5 AU; their perspective from the HELIOS orbits
  allow information to be gained about the three-dimensional shapes
  of specific mass ejections viewed both by coronagraphs and HELIOS;
  the global view afforded by the spacecraft photometers can image the
  mass ejection from within and thus relate in situ measurements to the
  shape of the whole structure.

---------------------------------------------------------
Title: Helios images of solar mass ejections
Authors: Jackson, B. V.; Leinert, C.
1985JGR....9010759J    Altcode:
  The zodiacal light photometers on board the Helios B spacecraft
  are used to form images of solar mass ejection transients in the
  interplanetary medium. Several aspects of these data are unique:
  (1) They trace shapes of solar mass ejections observed near the
  solar surface in coronagraph images to distances at least as great
  as 0.5 AU using electron Thomson scattering. (2) When compared with
  earth-based observations, the Helios data allow determination of the
  three-dimensional shapes of the ejections. (3) The global viewpoint
  of the Helios spacecraft photometers allows imaging of mass ejections
  heating toward the spacecraft and then observations from within the
  ejection. Excess masses (above the ambient level) are determined for
  several ejections, and we find that they are generally comparable to
  or somewhat larger than masses obtained by coronagraph observations
  of ejections when they are closer to the sun.

---------------------------------------------------------
Title: Imaging of Coronal Mass Ejections by the HELIOS Spacecraft
Authors: Jackson, B. V.
1985SoPh..100..563J    Altcode:
  The zodiacal light photometers on board the HELIOS spacecraft can be
  used to form images of coronal mass ejections in the interplanetary
  medium. Several aspects of these data are unique: they trace coronal
  mass ejections using Thomson scattering techniques to distances from
  the Sun greater than 0.5 AU; their perspective from the HELIOS orbits
  allow information to be gained about the three-dimensional shapes
  of specific mass ejections viewed both by coronagraphs and HELIOS;
  the global view afforded by the spacecrafts photometers can image
  the mass ejection from within and thus relate in situ measurements
  to the shape of the whole structure. To date, the HELIOS photometers
  have been used to study coronagraph-observed mass ejections including
  those which originate at the Sun on 7 May, 24 May, and 27 November,
  1979, and 21 May, 18 June, 29 June, and 6 November, 1980. Masses of
  ejections determined from these data are generally a few times larger
  than masses determined from SOLWIND coronagraph images.

---------------------------------------------------------
Title: Helios spacecraft and earth perspective observations of three
    looplike solar mass ejection transients
Authors: Jackson, B. V.; Howard, R. A.; Sheeley, N. R., Jr.; Michels,
   D. J.; Koomen, M. J.; Illing, R. M. E.
1985JGR....90.5075J    Altcode:
  Three looplike mass ejection transients observed from earth with the
  SOLWIND coronagraph and the solar maximum mission coronagraph are
  imaged by Helios spacecraft zodiacal light photometers. Because the
  Helios spacecraft are not earth orbiting, views of these ejections
  from the two perspectives allow conclusions to be drawn about their
  three-dimensional shapes. The mass ejection of May 24, 1979, in
  Helios data is concentrated in an outer structure followed by bright
  features separated by a region of depleted material. The ejections of
  June 18 and 29, 1980, appear restricted in position angle in Helios
  observations to less and the same, respectively, as in coronagraph
  observations. The observations imply that the ejections essentially
  retain their basic structure and speed out to heights (0.2-0.4 AU)
  observed by the Helios spacecraft.

---------------------------------------------------------
Title: Use of interplanetary scintillation for Earth space environment
    and geomagnetic forecasting
Authors: Jackson, B. V.; Rickett, B. J.
1985ucsd.reptQ....J    Altcode:
  A comparison is presented between solar wind velocities determined
  from IPS (Interplanetary Scintillation) observations made from 1973 to
  1981 with those measured in situ by spacecraft instruments. The IPS
  method is indirect but it provides reasonably accurate estimates of
  the large scale and slowly varying velocity structures in the solar
  wind. Thus the corotating solar wind streams typical of 1973 to 1975
  (declining and low solar activity) are well estimated; the slower
  average speed typical of 1979 to 1981 was also well estimated. However,
  the transient increases during this period of high solar activity were
  often not detected. The difficulties of interpretation are offset by
  the capacity to monitor the solar wind speed out of the ecliptic and
  over long periods of the time without the expense of a spacecraft.

---------------------------------------------------------
Title: The Mass Distribution of Coronal Mass Ejections
Authors: Jackson, B. V.; Howard, R. A.; Koomen, M. J.; Michels, D. J.;
   Sheeley, N. R., Jr.
1985BAAS...17..636J    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Brightness of the Interplanetary Medium in Thomson
Scattering from 0.3 to 1.0 AU: Comparison with a View from Helios B
Authors: Venkataraman, A.; Hudson, H. S.; Jackson, B. V.
1985BAAS...17..638V    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Helios observations of the earthward-directed mass ejection
    of 27 November, 1979
Authors: Jackson, B. V.
1985SoPh...95..363J    Altcode:
  The Helios spacecraft zodiacal light photometers are used to observe
  the earthward-directed solar mass ejection transient of 27 November,
  1979 described by Howard et al. (1982) that completely circles the Sun
  in coronagraph observations. At this time, Helios B was situated 30°
  east of the Sun-Earth line at 0.5 AU. The brightness increase moved
  outward directly along the Sun-Earth line over a period of approximately
  24 hr, indicating a strong collimation of the ejection. The outward
  motion and mass estimates of the ejected material from the photometers
  compared with near-Earth observations from IMP spacecraft show that
  at least a portion of the density increase observed at Earth on 29
  and 30 November was associated with this ejection.

---------------------------------------------------------
Title: Helios Observations of the Earthward-Directed Mass Ejection
    of 27 November 1979
Authors: Jackson, B. V.
1984BAAS...16..930J    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: A New UHF Antenna for IPS and Pulsar Observations
Authors: Kojima, M.; Coles, W. A.; Jackson, B. V.; Frehlich, R. B.
1984BAAS...16..517K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Helios Spacecraft and Earth Perspective Observations of the
    Loop-Like Solar Mass Ejection of 24 May 1979
Authors: Jackson, B. V.
1984BAAS...16..453J    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Energetics and Interplanetary Effects of the August 14 and 18,
1979 Solar Flares: Summary of Observations Made during the Smy/stip
    Event no.
Authors: Kane, S. R.; Bird, M. K.; Domingo, V.; Gapper, G. R.; Green,
   G.; Hewish, A.; Howard, R. A.; Iwers, B.; Jackson, B. V.; Koren, U.;
   Kunow, H.; McGuire, R. E.; Muller-Mellin, R.; Rompolt, B.; Sanahuja,
   B.; Sawant, H. S.; Stewart, R. T.; von Rosenvinge, T.; Wibberenz,
   G.; Zlobec, P.
1984sii..conf..175K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: IPS and Spacecraft Observations of the 14 August 1979 Mass
    Ejection Transient
Authors: Jackson, B. V.
1984sii..conf..169J    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Helios Images of a Coronal Mass Ejection Transient
Authors: Jackson, B. V.; Howard, R. A.; Koomen, M. J.; Michels, D. J.;
   Sheeley, N. R.
1983BAAS...15..705J    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Energetics and interplanetary effects of the August 14 and 18,
    1979 solar flares
Authors: Kane, S. R.; Bird, M. K.; Domingo, V.; Green, G.; Gapper,
   G. R.; Hewish, A.; Howard, R. A.; Iwers, B.; Jackson, B. V.; Koren, U.
1983STIN...8329164K    Altcode:
  The STIP Event No. 1, which covered the time interval August 14 - 18,
  1979, was characterized by two energetic flares: one on August 14
  (approximately 1243 UT) and the other on August 18 (approximately
  1400 UT). The hard X-ray, soft X-ray, optical, radio and energetic
  particle emissions from these flares and their interplanetary effects
  were observed with many instruments in space and on the ground. A
  summary of some of these observations is presented. The results of
  a preliminary analysis relevant to the acceleration of particles,
  coronal transients and evolution of shocks are as follows: (1) During
  the August 14 flare energetic particles were probably accelerated
  but could not escape the Sun in large numbers. On the other hand,
  during the August 18 flare the acceleration of high energy particles
  occurred relatively high in the corona, from whence they could easily
  escape into interplanetary space but could not penetrate down to the
  lower altitudes in the solar atmosphere in large numbers. (2) The
  kinetic energy of the coronal transient associated with the August 14
  flare was much larger than the total energy of energetic electrons,
  indicating an additional energy source for the transient. (3) The shock
  associated with the August 18 flare extended to greater than 2 (3.14)
  steradians. The shock maintained its speed from the flare site to a
  distance of approximately 35 R and then decelerated to a distance of
  approximately 1 AU as approximately R to the minus 0.8 power.

---------------------------------------------------------
Title: Kinematical Analysis of Flare Spray Ejecta Observed in
    the Corona
Authors: Webb, D. F.; Jackson, B. V.
1981SoPh...73..341W    Altcode:
  The mass ejection event on 17 January 1974 was a classsic spray
  associated with a flare from an over the limb region. The
  structure of the accompanying coronal transient was typical
  of well-observed mass ejections, with coronal loops and a
  forerunner racing ahead of the rising prominence. Observations
  in Hα, soft X-ray, white light and radio wavelengths allowed
  us to track both cool (T<SUB>e</SUB>∼10<SUP>4</SUP> K) and hot
  (T<SUB>e</SUB>&gt;10<SUP>6</SUP> K) material from limb de-occultation
  to 6R<SUB>⊙</SUB>. We determined the kinematics and thermodynamics
  of the internal material, and the overall mass and energy budget
  of the event. The majority of the mass and energy was linked with
  coronal material, but at least 20% of the ejected mass originated as
  near-surface prominence material. We conclude that the upper part of
  the prominence was being continuously heated to coronal temperatures
  as it rose through the corona. Above ∼2R<SUB>⊙</SUB> nearly all
  of the material was completely ionized. The primary acceleration of
  the prominence occurred below 3.5 × 10<SUP>4</SUP> km with all of the
  material exhibiting constant velocity above 1.5R<SUB>⊙</SUB>. We found
  evidence that a moving type IV burst, indicative of strong magnetic
  fields, was associated with the upper part of the prominence. Our
  observations suggest that both the cool and hot material were acted
  upon by a similar, continuous force(s) to great heights and over a
  long time interval. We find that the observations are most consistent
  with magnetic propulsion models of coronal transients.

---------------------------------------------------------
Title: A Comparison of Type-Iii Metric Radio Bursts and Global Solar
    Potential Field Models
Authors: Jackson, B. V.; Levine, R. H.
1981SoPh...73..183J    Altcode:
  We compare evidence of coronal magnetic fields from polarized metric
  type III radio bursts with (a) global potential field models, (b)
  direct averages of the observed photospheric magnetic field, and
  (c) Hα synoptic charts. The comparison clearly indicates both that
  the principal aspects of type III burst radiation are understood and
  that global potential field models are a significantly more accurate
  representation of coronal magnetic field structure than either the
  large-scale photospheric field or Hα synoptic charts.

---------------------------------------------------------
Title: Forerunners - Early Coronal Manifestations of Solar Mass
    Ejection Events
Authors: Jackson, B. V.
1981SoPh...73..133J    Altcode:
  Coronal ejection transients viewed with the white light coronagraph on
  Skylab are studied from the times of their very earliest manifestations
  for clues to their origin. Excess coronal mass with a configuration
  like that of the eventual transient is seen in twelve events prior to
  the transient's associated near-surface Hα eruption or flare. In seven
  of the events, data are adequate to observe the rates of outward mass
  motion of coronal material prior to their surface manifestations. The
  observations place severe constraints on different solar mass ejection
  mechanisms because they spread the process responsible for the ejection
  over a larger region of the corona and over a longer period of time
  than normally considered. The observations suggest the corona is an
  active participant in the ejection that begins with the acceleration
  of the outer portion of a preexisting structure and ends with the
  obvious surface manifestation.

---------------------------------------------------------
Title: The three-dimensional structure of the solar wind from radio
    scintillations
Authors: Jackson, B. V.; Nagendran, A.
1981ucsd.rept.....J    Altcode:
  Since 1972 the UCSD 74 MHz radio observatory has continuously monitored
  the solar wind using the method of interplanetary scintillation
  (IPS). The two reports presented here bear on the problems involved
  in tracing the fast changing three dimensional structure of the solar
  wind from the solar surface out to the vicinity of the Earth. The
  interplanetary scintillation technique is a radio propagation method
  for studying the velocity and small scale (approximately 100 to 1000
  km) turbulence in the solar wind. The signals are cross-correlated from
  three spaced antennas to yield time offsets from which the speed of the
  scintillation pattern can be deduced. Comparisons of IPS observations
  with spacecraft measurements have shown excellent agreement when the IPS
  source lies in the ecliptic plane. Furthermore, observations can be made
  in the direction of many radio sources (almost) simultaneously so as
  to generate a three-dimensional map of the solar wind. The eight-year
  data base is important for correlative studies throughout the solar
  cycle. In our analysis we emphasize three time scales are emphasized:
  (1) the solar cycle evolution of six month average velocity structures;
  (2) studies of one solar rotation duration; and (3) variations in the
  solar wind structure on time scales of a few days.

---------------------------------------------------------
Title: An Active Region-Type III Burst Association
Authors: Jackson, B. V.
1981BAAS...13..861J    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar Cycle Variation of IPS Transients Observed Near Earth
Authors: Jackson, B. V.
1980BAAS...12..920J    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Kinematical Analysis of a Spray Observed in the Corona
Authors: Webb, D. F.; Jackson, B. V.
1980BAAS...12..527W    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: A Comparison of Type III Metric Radio Bursts and Global Solar
    Potential Field Models
Authors: Jackson, B. V.; Levine, R. H.
1980BAAS...12..515J    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The preflare state
Authors: van Hoven, G.; Barbosa, D. D.; Birn, J.; Cheng, C. -C.;
   Hansen, R. T.; Jackson, B. V.; Martin, S. F.; McIntosh, P. S.;
   Nakagawa, Y.; Anzer, U.
1980sfsl.work...17V    Altcode: 1980sofl.symp...17V
  The accumulation, storage and irreversible release of the free
  energy necessary for a solar flare are discussed on the basis of data
  obtained from the Apollo Telescope Mount on Skylab and other pertinent
  sources. Skylab and OSO 7 observations of possible flare precursors
  and flare evolution are presented, and the evolution of the flare of
  Sept. 5, 1973, the most completely observed flare of the Skylab program,
  is described in detail, with account given to magnetic structures and
  H alpha radiation. Theories of the preflare state are then reviewed,
  with attention given to the force-free fields and coronal arcades,
  thermal and magnetic structures and the MHD stability of coronal loops.

---------------------------------------------------------
Title: The association of type III bursts and coronal transient
    activity
Authors: Jackson, B. V.; Dulk, G. A.; Sheridan, K. V.
1980IAUS...91..379J    Altcode:
  A broad peak in the number of isolated type III bursts occurring
  about five hours prior to large H-alpha solar flares is reported. It
  is suggested that the increase and subsequent decrease in type III
  activity indicates a new phase in the coronal adjustment to the
  long-term addition of energy, with some of the energy going into
  lifting the plasma and some possibly into the kinetic energy of moving
  plasma. The peak in the type III activity may signal the beginning
  of outward coronal plasma motion. The peak may thus be studied for
  clues to the energy input mechanism or mechanisms responsible for mass
  ejection transients.

---------------------------------------------------------
Title: Evidence for a peak in the number of isolated Type III bursts
    prior to large solar flares
Authors: Jackson, B. V.; Sheridan, K. V.
1979PASA....3..383J    Altcode: 1979PASAu...3..383J
  Evidence for a broad maximum in the number of isolated metric-wave Type
  III bursts prior to the large H alpha solar flares observed between May
  1973 and February 1974 is reported. The time distribution of isolated
  Type III bursts within 12.6 h of each of the 111 solar flares of
  importance 1 or greater recorded during the period is shown to peak
  approximately 5 h before the time of flare maximum, most markedly
  in the case of bursts with projected positions near the solar flare
  position. The examination of H alpha, X-ray and magnetogram data in
  the vicinity of the flare implies a purely coronal storage and release
  mechanism for the flare energy. The peak of Type III burst activity
  is thus suggested as a good indicator of coronal energy input and
  storage near the time of a large solar flare, although not a reliable
  flare predictor.

---------------------------------------------------------
Title: Comparison of radioheliograph, coronagraph and K-coronameter
    observations of a coronal streamer
Authors: Jackson, B. V.; Dulk, G. A.; Sheridan, K. V.
1979PASA....3..387J    Altcode: 1979PASAu...3..387J
  A comparison is made of observations of a bright coronal streamer made
  with an 80 MHz radioheliograph, a K-coronameter, and the Skylab white
  light coronagraph. The values of polarization radiance were used to
  derive a coronal density model, and an alternative model was calculated
  for a streamer density distribution such as given by Newkirk (1961);
  neither model fits the radioheliograph observations well. In particular,
  radio brightnesses are lower than expected on the basis of white light
  or EUV data, at least at low heights near the plasma level. With regard
  to this discrepancy, fundamental questions about the nature of the
  corona and wave propagation through a streamer structure are considered.

---------------------------------------------------------
Title: Forerunners: outer rims of solar coronal transients.
Authors: Jackson, B. V.; Hildner, E.
1978SoPh...60..155J    Altcode:
  The large loop or blob-like transient events viewed in the white-light
  corona are rimmed by broad regions where the density is slightly
  enhanced above the pre-transient corona. Every one of the Skylab events
  studied for which sufficiently good Skylab coronagraph coverage is
  available shows this effect. The upper boundaries of these `forerunners'
  blend gradually into the background corona 1 to ≥2R<SUB>⊙</SUB>
  above the transients' leading edges. In any single event, the coronal
  mass enhancement represented by the forerunner comprises up to 25% of
  the total excess mass present in the coronagraph's field of view and
  includes a much larger volume of the corona than previously attributed
  to the underlying transient. We have not yet seen a forerunner without
  an accompanying transient. Clearly, forerunners must be reckoned
  with in any proposed models of discrete outward coronal mass motions,
  because they indicate the presence of disturbed corona far ahead of
  the denser portions of the event.

---------------------------------------------------------
Title: A possible association of solar type III bursts and white
    light transients.
Authors: Jackson, B. V.; Sheridan, K. V.; Dulk, G. A.; McLean, D. J.
1978PASA....3..241J    Altcode: 1978PASAu...3..241J
  The possibility is considered whether type III bursts are in any
  way related to mass ejections indicated by white-light coronal
  transients. Forty coronal transients observed from Skylab are used
  to investigate the possible association with meter-wave type III
  bursts. It is shown that the time interval 5 to 10 hr prior to the
  time of a transient observation has at least 2.5 times the number of
  type III bursts expected and that the peak in the number of type III
  bursts also occurs in this time interval when the data are divided into
  various groupings. Positions of type III bursts are found usually to be
  located within 20 deg of the solar position angle of the corresponding
  transients.

---------------------------------------------------------
Title: Radio observations of a massive, slow moving ejection of
    coronal material
Authors: Sheridan, K. V.; Jackson, B. V.; McLear, D. J.; Dulk, G. A.
1978PASA....3..249S    Altcode: 1978PASAu...3..249S
  No abstract at ADS

---------------------------------------------------------
Title: Coronal Mass Increases Prior to Surface Hα Eruptions from
    the Sun.
Authors: Jackson, B. V.
1977BAAS....9..569J    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Atmospheric water vapor at South Pole
Authors: Smythe, William D.; Jackson, Bernard V.
1977ApOpt..16.2041S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Open magnetic structures on the sun.
Authors: Levine, R. H.; Altschuler, M. D.; Harvey, J. W.; Jackson,
   B. V.
1977ApJ...215..636L    Altcode:
  High-resolution harmonic analysis of the solar magnetic field has
  been used succesfully to calculate the geometry of open magnetic field
  lines in the solar corona. Comparison of the loci of open-field-line
  footpoints with solar X-ray photographs shows that all the coronal
  holes during two solar rotations are successfully represented, including
  details of their evolution. Some open magnetic configurations derived in
  the calculations precede by up to one solar rotation the manifestation
  of coincident dark areas on the X-ray photographs. The only other
  areas that contribute open field lines to the corona are separations
  between active-region loop systems. By varying the radius at which
  field lines are forced to be open in the calculation, it is possible to
  reproduce more closely the surface configuration of particular coronal
  holes. Comparison of the size of X-ray holes with the fraction of the
  solar surface covered by open field lines leads to the conclusion
  that a significant part of the area of coronal holes must contain
  closed magnetic fields. Comparison of open field lines which lie in
  the equatorial plane of the sun with solar-wind data indicates that
  eventual high-speed solar-wind streams are associated with those parts
  of open magnetic structures that diverge the least.

---------------------------------------------------------
Title: Physical properties of a polar coronal hole from 2 to 5 R sun.
Authors: Munro, R. H.; Jackson, B. V.
1977ApJ...213..874M    Altcode:
  Observations with a white-light coronagraph aboard Skylab are used
  to determine the boundaries of a coronal hole in the northern polar
  region and the three-dimensional density structure within the hole
  between heights of 2 and 5 solar radii. The boundary of the hole is
  found to be essentially axisymmetric about the polar axis, nearly
  radial from 3 to 6 solar radii, and located near 25 deg latitude at
  these heights. The radiances arising from the hole are interpreted as
  resulting from an axisymmetric density distribution whose logarithmic
  radial gradient is independent of position within the hole and whose
  magnitude increases with angular distance away from the hole's axis. The
  velocity distribution within the hole is obtained from the continuity
  equation by assuming that the particle flux flowing outward in the hole
  is similar to that measured for high-speed solar-wind streams at 1 AU,
  and it is shown that the transition from subsonic to supersonic flow
  occurs between 2.2 and 3 solar radii.

---------------------------------------------------------
Title: Forerunners Rim Solar Transients.
Authors: Jackson, B. V.
1977BAAS....9..368J    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: A Polar Coronal Hole: I. The Three Dimensional Boundary
Authors: Jackson, B. V.
1976BAAS....8..325J    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Cool-Star Spectrum Synthesis
Authors: Jackson, Bernard V.
1970BAAS....2..322J    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The rotational temperature of a TiO band in the spectrum of
    R Hydrae.
Authors: Keller, C. F.; Jackson, B. V.; Poland, A. I.; Peery,
   B. F., Jr.
1970A&A.....4..415K    Altcode:
  A procedure is presented for the determination of a rotational
  temperature from observations of the (1.0) ?`8 TiO band. The method is
  based upon comparison between accurately measured wavelengths of blended
  absorption features in the band and corresponding wavelengths in the
  computed band proffle. The rotational temperature found from McDonald
  coude' spectrograms of R Hydrae is Trot = 1430 290 0K. Key words:
  R Hydrae, long period variable - molecular spectroscopy, TiO-temperature

---------------------------------------------------------
Title: Cool Star Spectrum Synthesis.
Authors: Jackson, Bernard Vernon
1970PhDT.........6J    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: A Procedure for Determining Molecular Rotational Temperature.
Authors: Jackson, Bernard V.; Peery, Benjamin F., Jr.
1968AJS....73Q..20J    Altcode:
  A molecular rotational "line" in stellar spectra is usually a blend
  of chance wavelength-coincidences of several transitions, some out
  of states of low rotational energy and others out of states of high
  rotational energy. The wavelength of minimum intensity in such an
  unresolved absorption blend will be temperature dependent; the relative
  strengths of the blending contributors depend upon the populations of
  the lower rotational states. A critical comparison of the wavelengths
  of intensity minima in the observed spectrum and in profiles computed
  with various temperatures leads to a rotational temperature. We have
  produced theoretical profiles by use of the Minnaert semiempirical
  formula 1 1 1 R(N) Re r(N) where R (N) is the depth of the absorption in
  the band at wavelength N, Re the maximum depth (here taken as 1), and T
  (N) the optical depth due to all overlapping rotational lines at N. We
  assume a Gaussian absorption coefficient for each transition, weighted
  according to its H6nl-London strength factor and the Boltzmann factor
  at the temperature used. A Gaussian width is chosen that reproduces
  the level of resolution shown on a microdensitometer tracing of
  the stellar spectrum. There is no need for an intensity tracing in
  this procedure. The procedure has been applied to the (0,1) band of
  the 37r - 37r green a system of TiO in the spectrum of a Herculis
  (10 Amm). The best fit of measured and calculated wavelengths of the
  absorption minima yields Taot=25000+1500K.