HR: 14:30h
AN: SH33A-05    [Abstracts]
TI: A Search for Relativistic High-Energy Protons From the Extreme Solar Flares of 2000-03
AU: * Didkovsky, L V
EM: leonid@usc.edu
AF: USC, 835 W. 37th St, Los Angeles, CA 90089-1341 United States
AU: Jones, A R
EM: arjones@usc.edu
AF: USC, 835 W. 37th St, Los Angeles, CA 90089-1341 United States
AU: Judge, D L
EM: judge@usc.edu
AF: USC, 835 W. 37th St, Los Angeles, CA 90089-1341 United States
AU: Gurman, J
EM: gurman@gsfc.nasa.gov
AF: GSFC, NASA Goddard Space Flight Center, Greenbelt, MD 20771 United States
AU: Gangopadhyay, P
EM: pradip@usc.edu
AF: USC, 835 W. 37th St, Los Angeles, CA 90089-1341 United States
AU: Rhodes, E
EM: erhodes@almaak.usc.edu
AF: USC, 835 W. 37th St, Los Angeles, CA 90089-1341 United States
AU: Tsurutani, B T
EM: Bruce.T.Tsurutani@jpl.nasa.gov
AF: USC/JPL, 4800 Oak Grove Dr, Pasadena, CA 91109 United States
AB: We applied a high-energy proton flux-measuring tool based on detection of the energy deposited by post-flare protons in the active silicon layers of the SOHO/EIT and TRACE CCDs to extract individual proton events from the Fe XII (19.5~ nm) spectral line solar images. Temporal profiles of proton flux for extreme solar flares of 2000--03, including their pre-flare, impulsive phase, and near-post-flare intervals were analyzed in proton energy ranges 40--400 MeV. Both time and energy distributions of post-flare protons may be interpreted as the presence of relativistic (c/3 -- c/2 velocity at 1 A.U.) protons in some post-flare fluxes.
DE: 1650 Solar variability
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2005 Joint Assembly