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

B.V. Jackson, J.M. Clover, A. Buffington P.Paul Hick, Center for Astrophysics and Space Sciences, University of California at San Diego, La Jolla, CA, USA Mario M. Bisi Institute of Mathematics and Physics, Aberystwyth University, Penglais Campus, Aberystwyth, Wales, UK. Masayoshi.

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

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  1. B.V. Jackson, J.M. Clover, A. BuffingtonP.Paul Hick, Center for Astrophysics and Space Sciences, University of California at San Diego, La Jolla, CA, USA Mario M. Bisi Institute of Mathematics and Physics, Aberystwyth University, Penglais Campus, Aberystwyth, Wales, UK 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 The January 2010 CMEs/ICMEs The August 2010 CMEs

  3. Jackson, B.V., et al., 2006, J. Geophys. Res., 111, A4, A04S91 SMEI A NASA – Air Force funded instrument Launch 6 January 2003 1 gigabyte/day; now ~3 terabytes  Sun C1 C2 C3 Sun | V Simultaneous images from the three SMEI cameras.

  4. Frame Composite for Aitoff Map Blue = Cam3; Green= Cam2; Red = Cam1 D290; 17 October 2003

  5. Heliospheric direct images (differenced) SMEI difference images

  6. 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

  7. 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

  8. Heliospheric 3-D 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.

  9. 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 28 May 2003 halo CME as viewed from 15º above the ecliptic plane about 30º east of the Sun-Earth line. SMEI density 3D reconstruction of the 28 May 2003 halo CME as viewed from 30º above the ecliptic plane about 30º east of the Sun-Earth line. SMEI density (remote observer view) of the 28 May 2003 halo CME

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

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

  12. 2010 January CME events LASCO C3 coronagraph views Late 14 January CME 17 January CME

  13. 2010 January CME events STEREO-B in-situ analysis

  14. 2010 January CME events SMEI analysis Brightness difference Density ecliptic cut

  15. 2010 January CME events SMEI analysis Brightness difference Density ecliptic cut

  16. 2010 January CME events STEREO-B in-situ analysis

  17. 2010 January CME events LASCO C3 coronagraph simulation Late 14 January CME 17 January CME

  18. 2010 January CME events CME loop density structure Density meridional cut Density ecliptic cut

  19. 2010 January CME events CME loop density structure Density meridional cut Density ecliptic cut

  20. 2010 January CME events CME loop density structure Density meridional cut Density ecliptic cut

  21. 2010 January CME events CME loop density structure Density meridional cut Density ecliptic cut

  22. 2010 January CME events CME loop density structure Density meridional cut Density ecliptic cut

  23. A new larger computer (48 GBytes RAM) has just become available to the UCSD group at the Center for Astrophysics and Space Sciences This allows the 3D “exploratory” reconstruction of the heliosphere in a way that has never-before been possible: unprecedented 3D resolutions both spatially and temporally. This higher-resolution analysis is shown to advantage on the CMEs of 1-5 August 2010. Masayoshi

  24. There is sufficient line-of-sight coverage to enable a much-higher 3D reconstruction of the heliosphere near the Earth. To the left is an old ecliptic cut for the August CMEs, and to the right a plot at the same time for the numbers of line-of-sight crossings per resolution element. These numbers far exceed the necessary numbers required especially near Earth. August 2010 Density Ecliptic Cut Line-of-sight coverage Masayoshi

  25. To the left, an analysis with digital 3D resolutions of 6.7º in latitude and longitude and 0.5-day temporal. To the right, an analysis with digital 3D resolutions of 3.3º in latitude and longitude and 0.25-day temporal. The solar wind heights reconstructed are commensurate with the higher resolutions of: at left, 0.10 AU, and at right, 0.05 AU. Noise (perhaps caused by lunar light contamination) August 2010 August 2010 Density Ecliptic Cut Density Ecliptic Cut Masayoshi

  26. To the left, an analysis with digital 3D resolutions of 6.7º in latitude and longitude and 0.5-day temporal. To the right, an analysis with digital 3D resolutions of 3.3º in latitude and longitude and 0.25-day temporal. The solar wind heights reconstructed are commensurate with the higher resolutions of: at left, 0.10 AU, and at right, 0.05 AU. August 2010 August 2010 Density Meridional Cut Density Meridional Cut Masayoshi

  27. In-situ analysis from Wind densities  CME onset 6.7º in latitude and longitude and 0.50-day temporal 3D digital resolution. 3.3º in latitude and longitude and 0.25-day temporal 3D digital resolution (a somewhat higher correlation is found).  CME onset Masayoshi

  28. IPS analysis and forecasts - current STELab data sets Forecast Forecast

  29. 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… 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 ICME doesn’t really look like a magnetic loop. It may extend to Earth. The January 2010 and August 2010 CMEs are examples of what works with the analysis We are getting better!

  30. 2010 January CME events CME loop density structure Density meridional cut Density ecliptic cut

  31. 2010 January CME events CME loop density structure Density meridional cut Density ecliptic cut

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