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B.V. Jackson, P.P. Hick, A. Buffington, M.M. Bisi, J.M. Clover, S. Hamilton

The Solar Mass Ejection Imager (SMEI) 3D-reconstruction of density enhancements behind interplanetary shocks. B.V. Jackson, P.P. Hick, A. Buffington, M.M. Bisi, J.M. Clover, S. Hamilton Center for Astrophysics and Space Sciences, University of California at San Diego, LaJolla, CA, USA.

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B.V. Jackson, P.P. Hick, A. Buffington, M.M. Bisi, J.M. Clover, S. Hamilton

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  1. The Solar Mass Ejection Imager (SMEI) 3D-reconstruction of density enhancements behind interplanetary shocks B.V. Jackson, P.P. Hick, A. Buffington, M.M. Bisi,J.M. Clover, S. Hamilton Center for Astrophysics and Space Sciences, University of California at San Diego, LaJolla, CA, USA and M. Tokumaru, K. Fujiki Solar-Terrestrial Environment Laboratory, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Japan http://smei.ucsd.edu/ http://ips.ucsd.edu/ Masayoshi

  2. Lots of Data!! Launch 6 January 2003 1 gigabyte/day; now ~3 terabytes  Sun C1 C2 C3 Sun | V Simultaneous images from the three SMEI cameras.

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

  4. Brightness fall-off with distance

  5. STELab IPS Heliospheric Analyses IPS line-of-sight response STELab IPS array near Fuji

  6. Heliospheric 3D-reconstructions 30º LOS Weighting 60º 90º The outward-flowing solar wind structure follows very specific physics as it moves outward from the Sun Thomson scattering

  7. SMEI 3D reconstruction of the 28 October (Halloween Storm) 2003 CME. LASCO C2 coronagraph image. SMEI 3D-reconstruction.

  8. Recent higher-resolution SMEI PC 3D reconstructions show the CME sheath region as well as the central dense core 28 October 2003 CME “Halloween storm” ICME shock Ecliptic cuts

  9. 28 October 2003 CME/ICME shock density Meridional cuts Shock density enhancement volumetric mass The shock density enhancement of the 28 October 2003 ICME is present over only a tiny portion of the heliosphere!

  10. 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 (remote observer view) of the 28 May 2003 halo CME

  11. 2003 May 27-28 CME events CME masses

  12. 27-28 May 2003 CME event period IPS Velocity and SMEI proton density reconstruction of the 27-28 May 2003 halo CME sequence. Reconstructed and Windin-situ densities are compared with over one Carrington rotation.

  13. 20 January 2005 CME shock SMEI Ulysses .  Ulysses LASCO C2 coronagraph difference image. SMEI Hammer-Aitoff image of the whole sky The 20 January 2005 flare/ CME is associated with a very energetic (and prompt) SEP.

  14. 20 January 2005 CME shock ICME density from SMEI ACE SWEPAM density and velocity The bulk of the ICME mass of 3 x 1017 g reached 1 AU in about one day indicating an average speed for this mass of approximately 1600 km s-1, or a total kinetic energy for the CME of ~2 x 1033 ergs. A large shock was observed at Earth a day and a half following the CME onset at about 08:00 UT 20 January, 2005.

  15. 20 January 2005 CME shock shock density shock density Ecliptic cut Meridional cut In-situ shock From volumetric data determine mass flow past the spacecraft by measuring the density along the radial from Sun to Earth. From in situ data determine mass flow past the spacecraft by measuring the flux of material that has passed the spacecraft over time.

  16. 13 December 2006 CME shock SMEI fisheye image. LASCO C2 coronagraph difference image. SMEI fisheye difference image (image 12 hr earlier subtracted). The shock density enhancement of the 28 October 2003 ICME is present over only a tiny portion of the heliosphere!

  17. 13 December 2006 CME shock ACE SWEPAM density and velocity shock density shock density Ecliptic cut Meridional cut In-situ shock The shock density enhancement of the 13 December 2006 ICME is present to the South and North of Earth in greater extent than at Earth

  18. Shock event summary (measurements near Earth) All measurements in particles × 1013 cm-2. Brightness flux assumes a 10% helium abundance.

  19. Summary: The 3D SMEI analyses now show the extent of density enhancements behind shocks using these extremely- well calibrated brightness observations. The shock sheaths observed in the SMEI data are highly variable in latitudinal andlongitudinal extent. In SMEI, the shock density enhancementsanalyzed to datedo not show a uniform shell-like extent. Attempts to compare the density enhancements behind shocks from brightness and in situ measurements show not only the differences in the these two types of analyses, but also the great differences in the different instruments that measure proton density in situ.

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