HR: 0830h
AN: SH41B-0465    [PDF]
TI: Comparison between All-Sky Images Observed by Satellite SMEI and Simulations by using the HAF Solar Wind Model
AU: * Sun, W
EM: sun@jupiter.gi.alaska.edu
AF: Geophysical Institute, Geophysical Institute, UAF, 903 Koyukuk Dr., Fairbanks, AK 99775-7320 United States
AU: Deehr, C
EM: cdeehr@gi.alaska.edu
AF: Geophysical Institute, Geophysical Institute, UAF, 903 Koyukuk Dr., Fairbanks, AK 99775-7320 United States
AU: Fry, G
EM: gfry@expi.com
AF: Exploration Physics International, Inc., Exploration Physics International, Inc., Huntsville, AL 35806 United States
AU: Dryer, M
EM: Murray.Dryer@noaa.gov
AF: NOAA Space Environment Center, NOAA Space Environment Center, Boulder, CO 80305 United States
AU: Smith, Z
EM: Zdenka.Smith@noaa.gov
AF: NOAA Space Environment Center, NOAA Space Environment Center, Boulder, CO 80305 United States
AU: Akasofu, S
EM: sakasofu@iarc.uaf.edu
AF: International Arctic Research Center, UAF, International Arctic Research Center, UAF, Fairbanks, AK 99775 United States
AB: The Solar Mass Ejection Imager (SMEI) is a new satellite in sun-synchronous, low earth orbit with three wide-angle, white light photometers that provides a scan of the celestial sphere every orbit. By occulting the sun and correcting for other sources, the 0.1% of total light scattered from the increased plasma density associated with the flare-induced shock may be revealed. The first observations from SMEI were a series of eighteen frames acquired after two solar flares on May 27th and 29th, 2003. The interplanetary consequences of these flares were numerically modeled using the Hakamada-Akasofu-Fry (HAFv.2) kinematic solar wind model. Line-of-sight plasma densities due to the background solar wind and to the two shock fronts were calculated and displayed in the Hammer-Aitoff reference frame to enable direct comparison with the SMEI observations. Comparison of the HAFv.2 simulation with the SMEI observations clearly demonstrates that the model is necessary to aid in the identification of multiple shock-induced variations and to remove the contribution of the background solar wind from the SMEI observations.
DE: 2102 Corotating streams
DE: 2111 Ejecta, driver gases, and magnetic clouds
DE: 2139 Interplanetary shocks
DE: 7513 Coronal mass ejections
DE: 7519 Flares
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting