HR: 1340h
AN: SM33A-1110    [Abstracts]
TI: 3D Simulations of the Dynamics of the Relativistic Electrons in the Outer Radiation Belt
AU: * Subbotin, D
EM: subbotin@atmos.ucla.edu
AF: Department of Atmospheric and oceanic sciences, University of California, Los Angeles, 405 Hilgard Ave 7127 Math Sciences Bldg., Los Angeles, CA 90095-1565, United States
AU: Shprits, Y
EM: yshprits@atmos.ucla.edu
AF: Department of Atmospheric and oceanic sciences, University of California, Los Angeles, 405 Hilgard Ave 7127 Math Sciences Bldg., Los Angeles, CA 90095-1565, United States
AU: Thorne, R
EM: rmt@atmos.ucla.edu
AF: Department of Atmospheric and oceanic sciences, University of California, Los Angeles, 405 Hilgard Ave 7127 Math Sciences Bldg., Los Angeles, CA 90095-1565, United States
AB: The evolution of the relativistic electron fluxes in the radiation belts may be described by the 3D modified Fokker- Planck equation in terms of radial distance, pitch-angle, and energy. We present the results of numerical simulations using a 3D radiation belt diffusion code newly developed at UCLA. Quasi-liner diffusion coefficients are computed for resonance scattering by hiss waves inside plasmasphere, chorus waves outside plasmasphere and EMIC waves in the regions of plumes. We show that radial diffusion, pitch-angle scattering, energy diffusion, and various feedback mechanisms play an important role in the evolution of the relativistic electron fluxes in the radiation belts. Our results indicate that peaks in phase space density are produced by local acceleration in a distributed source region located near L~5.5. We also present comparison of the simulations with in-situ observations of the relativistic electron fluxes.
DE: 2753 Numerical modeling
DE: 2774 Radiation belts
SC: SPA-Magnetospheric Physics [SM]
MN: 2007 Fall Meeting