Solar Mass Ejection Imager SMEI 3 Dreconstructions of

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere Bernard V. Jackson, P. Paul Hick, Andrew Buffington, Mario M. Bisi, John M. Clover Center for Astrophysics and Space Sciences, University of California at San Diego, La. Jolla, CA, USA and Munetoshi Tokumaru Bernie Solar-Terrestrial Environment Laboratory, Nagoya University, Japan http: //smei. ucsd. edu/ http: //ips. ucsd. edu/ http: //stesun 5. stelab. nagoya-u. ac. jp/index-e. html/ Paul Andy Mario Masayoshi John Munetoshi CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere Introduction: SMEI and IPS remote-sensing data analyses Tomographic techniques used to determine Solar Wind 3 D structure (examples). Comparisons at Mars CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere http: //smei. ucsd. edu/ The Solar Mass Ejection Imager (SMEI) Mission (Solar Phys. , 225, 177 -207) B. V. Jackson, A. Buffington, P. P. Hick Center for Astrophysics and Space Sciences, University of California at San Diego, La. Jolla, 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 The SERP/STP Coriolis spacecraft G. M. Simnett, C. J. Eyles, M. P. Cooke, S. J. Tappin School of Physics and Space Research, University of Birmingham, UK at Vanden-berg T. Kuchar, D. Mizuno, D. F. Webb prior to flight. ISR, Boston College, Newton Center, MA P. A. Anderson Boston University, Boston, MA The SMEI baffles are S. L. Keil circled. The National Solar Observatory, Sunspot, NM large NRL R. E. Gold radiometer Windsat Johns Hopkins University/Applied Physics Laboratory, Laurel, MD is. Waltham on the top of the N. R. Space Science Dept. , Rutherford-Appleton Laboratory, Chilton, UK spacecraft. CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere Launch 6 January 2003 Data!! Lots of Data!! 1 gigabyte/day; now ~3. 5 terabytes Sun C 1 C 2 C 3 Sun | V Simultaneous images from the three SMEI cameras. CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere Frame Composite for Aitoff Map Blue = Cam 3; Green = Cam 2; Red = Cam 1 D 290; 17 October 2003 CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere SMEI first light composite image Composite all-sky map 2 Feb 2003 from the three SMEI cameras. CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere Brightness fall-off with distance A very tiny signal CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere 27 -28 May 2003 CME events brightness time series for select sky sidereal locations With all contaminant signals eliminated, SMEI brightness is shown with a long-term temporal base removed. Data points are obtained on each SMEI orbit every 102 -minutes, and the data here show a CME that has passed the Earth and is measured in situ. (1 S 10 = 0. 46 ± 0. 02 ADU) CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere “Cleaned brightness” from the 28 May 2003 halo CME at specific sidereal lines of sight over one 3 -hour period CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere STELab IPS Heliospheric Analyses IPS STELab line-of-sight IPS array response near Fuji CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere Density Turbulence v Scintillation index, m, is a measure of level of turbulence v Normalized Scintillation index, g = m(R) / <m(R)> • g > 1 enhancement in Ne • g 1 ambient level of Ne • g < 1 rarefaction in Ne (Courtesy of P. K. Manoharan) A scintillation enhancement with respect to the ambient wind identifies the presence of a region of increased turbulence/density and a possible CME along the line-of-sight to the radio source. CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere STELab IPS Heliospheric Analyses The newest STELab IPS array at Toyokawa - photo 17 February 2007 (October IPS Workshop see: http: //smei. ucsd. edu/ips_toyokawa. html) CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere 30º LOS Weighting 60º 90º Thomson scattering Heliospheric C. A. T. Analyses The outward-flowing solar wind structure follows very specific physics as it moves outward from the Sun CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere SMEI Heliospheric C. A. T. Analyses 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. A half-day difference CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere Heliospheric C. A. T. Analyses: example line-of-sight distribution for each sky location to form the source surface of the 3 D reconstruction. STELab IPS 13 14 July 2000 CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere 27 -28 May 2003 CME events SMEI density 3 D reconstruction of the 28 May 2003 halo CME as viewed from 15º above the ecliptic plane about 30º east of the Sun-Earth line. Jackson et al. , JGR. (2006) 111 (A 4): A 04 S 91 SMEI density (remote observer view) of the 28 May 2003 halo CME CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere 27 -28 May 2003 CME events CME masses Jackson et al. , JGR. (2006) 111 (A 4): A 04 S 91 CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere 27 -28 May 2003 CME event period density Earth in situ comparison SMEI proton density reconstruction of the May - June 2003 halo CME period compared with Wind over one Carrington rotation Jackson et al. , JGR. (2006) 111 (A 4): A 04 S 91 CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere SMEI Agreement with Sophisticated Modeling 27 -28 May 2003 CME events HAF Model Comparison Brightness from the 28 May 2003 halo CME 3 D reconstruction (left) and HAF model (right). Jackson et al. , JGR. (2006) 111 (A 4): A 04 S 91 CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere 28 October 2003 CME Northeast-directed ejecta is more-nearly earth-directed. Southward ejecta LASCO C 2 CME image to 6 Rs. SMEI enhanced Sky Map image and animation to 110º elongation. Jackson et al. , JGR. (2008) 113: A 00 A 15 C 2 image Southward ejecta SMEI C. A. T. Analysis CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere SMEI 3 D-reconstruction of the 28 October CME. The above structure has a mass of about 0. 5 1016 g excess in the sky plane but ~ 2. 0 1016 g excess at 60º (Vourlidas, private communication, 2004). Mass determination ~6. 7 1016 g excess and 8. 3 1016 g total for northward directed structure within the 10 e-cm-3 contour. SMEI C. A. T. Analysis CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere 28 October 2003 CME SMEI reconstructed density on 30`October at 03 UT 15 ecm-3 to 30 e- cc-3. IPS 3 D-reconstructed velocity at 03 UT viewed above 950 km s-1. CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere IPS and SMEI 3 D reconstruction of the 28 October 2003 CME IPS g-level data reconstruction of density from data obtained between 22 UT 28 and 7 UT 29 October 2003. The reconstruction time is ~3 UT. Mass ~6 1016 g Reconstruction from SMEI data on 03 UT 29 October 2003. Mass ~7 1016 g for the event northward portion CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere Recent higher-resolution SMEI PC 3 D reconstructions show the CME sheath region as well as the central dense core 28 October 2003 CME higher-resolution analysis shock Ecliptic cut Meridional cut SMEI C. A. T. Analysis CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere 28 October 2003 CME higher-resolution analysis Ecliptic cuts Meridional cuts SMEI C. A. T. Analysis CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere Solar Wind Pressure derived from the MGS Magnetometer at Mars Crider et al. , J. Geophys. Res. (2003) 108(A 12): 1461 CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere IPS 3 D Reconstruction 28 May 2003 ‘Halo’ CME event sequence Density derived from IPS | Jackson et al. , Solar Phys. (2007) 241: 385– 396 CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere IPS 3 D-Reconstruction 20 May – 05 June 2003, (28 May ‘Halo’ CME) Pressure derived from IPS at Mars Solar Wind Pressure (ρ = 2 X 106 n. V 2) Jackson et al. , Solar Phys. (2007) 241: 385– 396 CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere IPS 3 D-Reconstruction 12 September – 26 September 2002 period Density Pressure (ρ = 2 X 106 n. V 2) Jackson et al. , Solar Phys. (2007) 241: 385 – 396 CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere IPS solar wind pressure 3 D-reconstruction at Mars from 1999 - 2004 Time lags between ram pressure peaks (from a sample of 37 peaks). A positive shift indicates a lag in the IPS-derived pressure peak from that from MGS. CASS/UCSD-STELab AOGS_2009

Solar Mass Ejection Imager (SMEI) 3 D-reconstructions of the Inner Heliosphere Summary: a) SMEI allows derivation of global densities including that from CMEs at high spatial and temporal resolution using Thomson-scattering brightness. b) IPS allows derivation of global velocity, and through conversion of g-level to density – global densities, at low resolution from STELab data, including for CMEs. c) These have been combined to compare with Mars Global Surveyor magnetometer data where solar wind pressure have been derived from 1999 – 2004. Still needed – IPS velocity data from more radio sources in order to provide better velocity resolutions in comparison with derived global densities. CASS/UCSD-STELab AOGS_2009