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B.V. Jackson, J.M. Clover, A. Buffington and P. Paul Hick

The 3D Reconstruction of Heliospheric Density Using Thomson-Scattering Observations – Current Progress and Future Progress. B.V. Jackson, J.M. Clover, A. Buffington and P. Paul Hick Center for Astrophysics and Space Sciences, University of California at San Diego, La Jolla, CA, USA.

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B.V. Jackson, J.M. Clover, A. Buffington and P. Paul Hick

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  1. The 3D Reconstruction of Heliospheric Density Using Thomson-Scattering Observations – Current Progress and Future Progress B.V. Jackson, J.M. Clover, A. Buffington and P. Paul Hick Center for Astrophysics and Space Sciences, University of California at San Diego, La Jolla, CA, USA Masayoshi http://smei.ucsd.edu/ http://ips.ucsd.edu/

  2. Introduction: The data: The Solar Mass Ejection Imager (SMEI) 3D density reconstructions from SMEI brightness The test case – 30 May 2003 CMEs/ICMEs Recent programming enhancements and their use The future – near and distant

  3. Jackson, B.V., et al., 2004, Solar Phys., 225, 177 The Solar Mass Ejection Imager (SMEI) Mission -- Journal Article B. V. Jackson, A. Buffington, P. P. Hick Center for Astrophysics and Space Sciences, University of California at San Diego, LaJolla, CA. R.C. Altrock, S. Figueroa, P.E. Holladay, J.C. Johnston, S.W. Kahler, J.B. Mozer, S. Price,R.R. Radick, R. Sagalyn, D. Sinclair Air Force Research Laboratory/Space Vehicles Directorate (AFRL/VS), Hanscom AFB, MA G.M. Simnett, C.J. Eyles, M.P. Cooke, S.J. Tappin School of Physics and Space Research, University of Birmingham, UK T. Kuchar, D. Mizuno, D.F.Webb ISR, Boston College, Newton Center, MA P.A. Anderson Boston University, Boston, MA S.L. Keil National Solar Observatory, Sunspot, NM R.E. Gold Johns Hopkins University/Applied Physics Laboratory, Laurel, MD N.R. Waltham Space Science Dept., Rutherford-Appleton Laboratory, Chilton, UK The Coriolis spacecraft at Vandenberg prior to flight. The SMEI baffles are circled. The large NRL radiometer Windsat is on the top of the spacecraft.

  4. The Solar Mass Ejection Imager (SMEI) Jackson, B.V., et al., 2004, Solar Phys., 225, 177 Launch 6 January 2003 Sun C1 C2 C3 Sun 1 gigabyte/day; now ~4 terabytes Simultaneous images from the three SMEI cameras. A joint US Air Force - NASA Project

  5. Frame composite for Aitoff map Blue = Cam3; Green= Cam2; Red = Cam1 D290; 17 October 2003

  6. Jackson, B.V., et al., 2008, J. Geophys Res., 113, A00A15, doi:10.1029/2008JA013224 Heliospheric direct images (differenced) SMEI difference images

  7. UCSD editing sequences Jackson, B.V., et al., 2008, J. Geophys Res., 113, A00A15, doi:10.1029/2008JA013224 Aurora removal Aurora recognition and removal. How to know where the aurora is. How to remove it. Aurora removed by recognition of their signal on an orbit – temporal sequence map.

  8. Jackson, B.V., et al., 2008, J. Geophys Res., 113, A00A15, doi:10.1029/2008JA013224 27-28 May 2003 CME events brightness time series for select sky sidereal locations SMEI brightness with a long-term (~30 day) base removed. (1 S10 = 0.46 ± 0.02 ADU) SMEI data

  9. Heliospheric 3D-reconstructions Jackson, B.V., et al., 2008, Adv. in Geosciences 21, 339 30º LOS Weighting 60º 90º The outward-flowing solar wind structure follows very specific physics as it moves outward from the Sun Thomson scattering

  10. Heliospheric 3D reconstruction Jackson, B.V., et al., 2008, Adv. in Geosciences 21, 339 Line of sight “crossed” components on a reference surface. Projections on the reference surface are shown. These weighted components are inverted to provide the time-dependent tomographic reconstruction.

  11. Jackson, B.V., et al., 2008, J. Geophys Res., 113, A00A15, doi:10.1029/2008JA013224 2003 May 27-28 CME events SMEI density 3D reconstruction of the 27-28 May 2003 halo CMEs as viewed from 30º above the ecliptic plane about 30º west of the Sun-Earth line. SMEI density (remote observer view) of the 27-28 May 2003 halo CMEs LASCO C3

  12. Jackson, B.V., et al., 2008, J. Geophys Res., 113, A00A15, doi:10.1029/2008JA013224 2003 May 27-28 CME events CME mass

  13. A new larger computer (48 GBytes RAM) has just become available to the UCSD group at the Center for Astrophysics and Space Sciences (Thanks to funding from NSF AGS-1053766) This allows the 3D “exploratory” reconstruction of the heliosphere in a way that has never-before been possible: The whole of the SMEI data set cleaned of aurora Unprecedented 3D resolutions both spatially and temporally This higher-resolution analysis is shown to advantage on the CMEs observed to date. Masayoshi

  14. Jackson, B.V., et al., 2008, J. Geophys Res., 113, A00A15, doi:10.1029/2008JA013224 27-28 May 2003 CME event period 12-hour cadence, 7º x 7º lat, long SMEI proton density reconstruction for the 27-28 May 2003 halo CME sequence. Reconstructed and Windin-situ densities are compared over one Carrington rotation.

  15. Jackson, B.V., et al., 2008, J. Geophys Res., 113, A00A15, doi:10.1029/2008JA013224 27-28 May 2003 CME event period 12-hour cadence, 7º x 7º lat, long SMEI proton density reconstruction for the 27-28 May 2003 halo CME sequence. Reconstructed and Windin-situ densities are compared over one Carrington rotation.

  16. Jackson, B.V., et al., 2008, J. Geophys Res., 113, A00A15, doi:10.1029/2008JA013224 27-28 May 2003 CME event period Full SMEI data set, 6-hour cadence, 3º x 3º lat, long SMEI proton density reconstruction for the 27-28 May 2003 halo CME sequence. Reconstructed and ACE L2in-situ densities are compared over one Carrington rotation.

  17. 2010 January CME events SMEI analysis Brightness difference Density ecliptic cut 12-hour cadence, 7º x 7º lat, long

  18. 2010 January CME events SMEI analysis Brightness difference Density ecliptic cut 12-hour cadence, 7º x 7º lat, long

  19. 2010 January CME events STEREO-B in-situ analysis 12-hour cadence, 7º x 7º lat, long

  20. 2010 January CME events LASCO C3 coronagraph simulation Fall 2011 AGU special session: “How do heliospheric remote-sensing observations limit magnetic flux rope models?” Late 14 January CME 17 January CME 12-hour cadence, 7º x 7º lat, long

  21. The Future: Hinode Observing Proposal (HOP 187) 17 June 2011 00:00 - 06:00 UT (Jets in the solar wind) (Hinode XRT, EIS, SDO, LASCO C2, STEREO, IPS,SMEI) IPS/SMEI forecasting: Incorporation of in-situ measurements into the 3D reconstructions Future near-earth space imaging system concepts

  22. Hinode Observing Proposal (HOP 187) 17 June 2011 00:00 - 06:00 UT (Jets in the solar wind) (Hinode XRT, EIS, SDO, LASCO C2, STEREO, IPS,SMEI)

  23. Jets in Hinode XRT observations 3D IPS reconstruction program at the CCMC LASCO C2 Observations

  24. Jets in Hinode XRT observations Jet Coronagraph “Effect” 0.0 1.0 2.0 3.0 4.0 0.0 1.0 2.0 3.0 Jet X-ray Brightness

  25. Solar wind jet imaging using the enhanced SMEI 3D analysis Jet ? 6-hour cadence, 3º x 3º lat, long

  26. IPS/SMEI forecasting: SHINE workshop 2011 (CCMC, NICT evaluation)

  27. IPS analysis and forecasts - current STELab data sets Jackson, B.V., et al., 2010, Solar Phys., 265, 245-256. Forecast An Interplanetary Scintillation “Test System” real time at: http://ips.ucsd.edu/ In-situ measurements incorporated into the 3D analysis(enhances ability to forecast density and velocity changes) Forecast (Currently being evaluated for real time use at the CCMC, NICT (Japan) )

  28. Incorporation of in-situ data into the SMEI 3D reconstructions SMEI archival program is at the CCMC, SMEI real-time analysis a good future possibility in the next few months. (The SMEI auroral-removal algorithm program now takes only about 20 minutes to run, the lower-resolution tomography ~30 minutes. A script to put these and the visualizations together is being built.)

  29. Future near-earth space imaging system concepts (Wait)

  30. Near-Earth orbit Jackson, B.V., et al., 2010, “Lessons”, Solar Phys., 265, 257-275. Design concepts: ways to mitigate aurora / SAA Scanning Instrument inPolar Orbit (can look to within ~5º of Sun) SMEI Optic NASA “White Paper” Multiple Instrument heads on a single bus Multiple satellites

  31. ASI & other instrumentation accommodation Jackson, B.V., et al., 2010, “Lessons”, Solar Phys., 265, 257-275. NASA “White Paper” “Whole sky” ASI

  32. Summary: The 3D reconstruction fit to data: Allows a 3D reconstruction over time of most of the heliosphere for whatever structure is present - - CMEs, Co-rotating structures, shock sheaths, maybe the largest jets?... We’ve learned many things: The extent, shape, 3D mass of CMEs. The relationship of CME density to the in-situ measurements of these structures. The density of the 14 January 2010 gives the magnetic loop orientation for this event. Forecasts using this analysis for SMEI – coming along, IPS forecasts are here now. We are getting better!

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