HR: 0800h
AN: SM41A-1110    [Abstracts]
TI: The Halloween 2003 Storm's Effect on Trapped Electron Populations
AU: * Goodhue, A C
EM: agoodhue@ssl.berkeley.edu
AF: Physics and Astronomy Dept., Dartmouth College, Hanover, NH 03755 United States
AU: Hudson, M K
EM: mary.hudson@dartmouth.edu
AF: Physics and Astronomy Dept., Dartmouth College, Hanover, NH 03755 United States
AU: Hudson, H S
EM: hhudson@ssl.berkeley.edu
AF: Space Sciences Laboratory, University of California, Berkeley, Berkeley, CA 94720 United States
AU: McNab, M C
EM: michael.mcnab@aero.org
AF: Space Sciences Application Laboratory, The Aerospace Corp., Los Angeles, CA 90009 United States
AB: We have investigated the effects of the October and November 2003 solar energetic particle (SEP) events on trapped electron populations using data from the Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) in conjunction with the findings from the Solar, Anomalous, Magnetospheric Particle Explorer (SAMPEX). Immediately after the Halloween storm, RHESSI, saw an order of magnitude increase in the electron population in its low particle energy bin (less than 600 KeV); the population lingered for more than thirty days at L=1.9-2.2. The increase is caused by an inward transportation of trapped magnetospheric electrons from higher L values, and the decay is produced by pitch angle diffusion. Similar effects were seen by SAMPEX. However, the appearance of SEP's, whose energies are much greater and range up to 20 MeV, does not occur until months later, as these electrons are not pitch angle diffused as quickly as the lower energy population.
DE: 2700 MAGNETOSPHERIC PHYSICS
DE: 2720 Energetic particles, trapped
DE: 2784 Solar wind/magnetosphere interactions
DE: 2788 Storms and substorms
SC: SPA-Magnetospheric Physics [SM]
MN: 2004 AGU Fall Meeting