HR: 14:40h
AN: SM23C-04    [Abstracts]
TI: Solar Energetic Particle Contribution to the Particle Population at Geosynchronous Orbit
AU: * Richard, R L
EM: rrichard@igpp.ucla.edu
AF: Institute of Geophysics and Planetary Physics, University of California Los Angeles, 405 Hilgard Ave., Los Angeles, CA 90095-1567, United States
AU: El-Alaoui, M
AF: Institute of Geophysics and Planetary Physics, University of California Los Angeles, 405 Hilgard Ave., Los Angeles, CA 90095-1567, United States
AU: Ashour-Abdalla, M
AF: Institute of Geophysics and Planetary Physics, University of California Los Angeles, 405 Hilgard Ave., Los Angeles, CA 90095-1567, United States
AU: Ashour-Abdalla, M
AF: Department of Phyics and Astronomy, University of California Los Angeles, 405 Hilgard Ave., Los Angeles, CA 90095, United States
AU: Walker, R J
AF: Institute of Geophysics and Planetary Physics, University of California Los Angeles, 405 Hilgard Ave., Los Angeles, CA 90095-1567, United States
AB: To understand the formation of radiation belts it is important to assess the contributions of different upstream particle populations. Different sources can contribute to the energetic trapped particle population at geosyncronous orbit: Solar energetic particle (SEP) ions with energies above typical ring current energies (100 keV), lower energy SEPs below 100 keV that are accelerated to higher energies, and strongly accelerated solar wind particles. To study the entry and acceleration processes of SEPs we performed particle tracing calculations in the electric and magnetic fields from global magnetohydrodynamic (MHD) simulations of selected intervals. The weight of these particles in contributing to the observed particle flux is determined by using the flux observed by spacecraft in the solar wind. These calculations will be supplemented by trajectory calculations of lower energy particles to determine the dominant sources and acceleration models of energetic particles observed by geosynchronous spacecraft.
DE: 2716 Energetic particles: precipitating
DE: 2720 Energetic particles: trapped
DE: 2753 Numerical modeling
DE: 2774 Radiation belts
SC: SPA-Magnetospheric Physics [SM]
MN: 2007 Fall Meeting