1. CASS/UCSD ILWS 2009 SMEI 3D reconstructions of density behind 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 Masayoshi The Solar Mass Ejection Imager (SMEI) 3D-reconstruction of density enhancements behind interplanetary shocks http://smei.ucsd.edu/ http://ips.ucsd.edu/ and M. Tokumaru, K. Fujiki Solar-Terrestrial Environment Laboratory, Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Japan

2. CASS/UCSD ILWS 2009 SMEI 3D reconstructions of density behind shocks Simultaneous images from the three SMEI cameras. Lots of Data!! C1 C2 C3  Sun Sun | V 1 gigabyte/day; now ~3 terabytes Launch 6 January 2003

3. CASS/UCSD ILWS 2009 SMEI 3D reconstructions of density behind shocks Frame Composite for Aitoff Map Blue = Cam3; Green = Cam2; Red = Cam1 D290; 17 October 2003

4. CASS/UCSD ILWS 2009 SMEI 3D reconstructions of density behind shocks Brightness fall-off with distance

5. CASS/UCSD ILWS 2009 SMEI 3D reconstructions of density behind shocks STELab IPS Heliospheric Analyses STELab IPS array near FujiIPS line-of-sight response

6. CASS/UCSD ILWS 2009 SMEI 3D reconstructions of density behind shocks Heliospheric 3D-reconstructions Thomson scattering The outward-flowing solar wind structure follows very specific physics as it moves outward from the Sun LOS Weighting 30º 60º 90º

7. CASS/UCSD ILWS 2009 SMEI 3D reconstructions of density behind shocks SMEI 3D reconstruction of the 28 October (Halloween Storm) 2003 CME. SMEI 3D-reconstruction. LASCO C2 coronagraph image.

8. CASS/UCSD ILWS 2009 SMEI 3D reconstructions of density behind shocks 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 Ecliptic cuts shock

9. CASS/UCSD ILWS 2009 SMEI 3D reconstructions of density behind shocks

10. CASS/UCSD ILWS 2009 SMEI 3D reconstructions of density behind shocks The shock density enhancement of the 28 October 2003 ICME is present over only a tiny portion of the heliosphere! 28 October 2003 CME/ICME Meridional cuts Shock density enhancement volumetric mass shock density

11. CASS/UCSD ILWS 2009 SMEI 3D reconstructions of density behind shocks SMEI density (remote observer view) of the 28 May 2003 halo CME 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.

12. CASS/UCSD ILWS 2009 SMEI 3D reconstructions of density behind shocks 2003 May 27-28 CME events CME masses

13. CASS/UCSD ILWS 2009 SMEI 3D reconstructions of density behind shocks IPS Velocity and SMEI proton density reconstruction of the 27-28 May 2003 halo CME sequence. Reconstructed and Wind in-situ densities are compared with over one Carrington rotation. 27-28 May 2003 CME event period

14. CASS/UCSD ILWS 2009 SMEI 3D reconstructions of density behind shocks The 20 January 2005 flare/ CME is associated with a very energetic (and prompt) SEP. Ulysses . SMEI LASCO C2 coronagraph difference image. 20 January 2005 CME shock  Ulysses SMEI Hammer-Aitoff image of the whole sky

15. CASS/UCSD ILWS 2009 SMEI 3D reconstructions of density behind shocks 20 January 2005 CME shock ICME density from SMEI The bulk of the ICME mass of 3 x 10 17 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 10 33 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. ACE SWEPAM density and velocity

16. CASS/UCSD ILWS 2009 SMEI 3D reconstructions of density behind shocks 20 January 2005 CME shock Meridional cutEcliptic cut shock density 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. In-situ shock

17. CASS/UCSD ILWS 2009 SMEI 3D reconstructions of density behind shocks The shock density enhancement of the 28 October 2003 ICME is present over only a tiny portion of the heliosphere! 13 December 2006 CME shock SMEI fisheye image. LASCO C2 coronagraph difference image. SMEI fisheye difference image (image 12 hr earlier subtracted).

18. CASS/UCSD ILWS 2009 SMEI 3D reconstructions of density behind shocks 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 13 December 2006 CME shock Ecliptic cutIn-situ shock shock density Meridional cut ACE SWEPAM density and velocity

19. CASS/UCSD ILWS 2009 SMEI 3D reconstructions of density behind shocks ICME Brightness flux (SMEI) SOHO (CELIAS) WIND (SWE) ACE (SWEPAM) 28 May 20037.28.27.46.6 28 Oct 2003-- 20 Jan 20054.76.64.52.6 13 Dec 20064.12.61.81.0 Shock event summary (measurements near Earth) All measurements in particles × 10 13 cm -2. Brightness flux assumes a 10% helium abundance.

20. CASS/UCSD ILWS 2009 SMEI 3D reconstructions of density behind shocks 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 and longitudinal extent. In SMEI, the shock density enhancements analyzed to date do 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. Summary: