The 20 January 2005 CME Solar Mass Ejection Imager (SMEI) Analyses

Details The 20 January 2005 CME Solar Mass Ejection Imager (SMEI) Analyses The 20 January 2005 CME Solar Mass Ejection Imager (SMEI) Analyses

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsh33a0396j&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #SH33A-0396

Other

2111 Ejecta, Driver Gases, And Magnetic Clouds, 2139 Interplanetary Shocks, 2164 Solar Wind Plasma, 7513 Coronal Mass Ejections (2101), 7514 Energetic Particles (2114)

Scientific paper

Solar Mass Ejection Imager (SMEI) brightness measurements are analyzed to determine 3D volumetric densities for several CMEs including that of the 20 January 2005 CME. Here we present analyses of these 3D heliospheric volumetric solar wind density analyses. We use this system to measure the distribution of structure and provide a 3D mass of the ejecta associated with the large CMEs viewed in SMEI observations. In the case of the 20 January 2005 CME, the primary mass moves to the northwest of the Sun following the event observed earlier in LASCO coronagraph observations. There are two other very large coronal responses to the coronal energy input beginning around 6:30 UT near the time of CME onset. One of these is the large and extremely prompt Solar Energetic Particle (SEP) proton event observed at Earth beginning about 6:50 UT. Another response is an outward-propagating fast shock that arrives at Earth 34 hours following the event onset. A response that may be attributed to this shock is observed slightly more than 5 days following this at the Ulysses spacecraft situated 5.3 AU from the Sun, 17 degrees south of the ecliptic, and 27 degrees from the Sun-Earth line to the west. SMEI observes the white-light response of this shock at Earth in the interplanetary medium around the spacecraft, and limits the shock extent in 3D.

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