HR: 0800h
AN: SM21A-0317    [Abstracts]
TI: Storm-Dependent Radiation Belt Dynamics
AU: * Li, X
EM: lix@lasp.colorado.edu
AF: LASP and Dept. of Aerospace Engineering Sciences, University of Colorado 1234 Innovation Drive, Boulder, CO 80303, United States
AU: Tu, W
EM: Weichao.Tu@colorado.edu
AF: LASP and Dept. of Aerospace Engineering Sciences, University of Colorado 1234 Innovation Drive, Boulder, CO 80303, United States
AU: Chen, Y
EM: cheny@lanl.gov
AF: Space Science & Applications, ISR-1, Los Alamos National Laboratory, PO Box 1663, MS D466, Los Alamos, NM 87545, United States
AU: Reeves, G
EM: reeves@lanl.gov
AF: Space Science & Applications, ISR-1, Los Alamos National Laboratory, PO Box 1663, MS D466, Los Alamos, NM 87545, United States
AB: Outer radiation belt electrons have their largest variations during magnetic storms. Taking advantage of recently published phase space density (PSD) data as a function of L* and time, we have developed a comprehensive radial diffusion model, in which both the electron lifetime and source rate are included and parameterized as a function of geomagnetic indices. The PSD data at L*=6 is used as the outer boundary source and the modeled results are directly compared with the PSD data at L*=4. We conclude that the main acceleration mechanism, inward radial diffusion vs in situ acceleration, responsible for the enhancement of outer belt electrons at L*=4 is storm-dependent: in one storm, the enhancement of outer radiation belt electrons can be well explained by inward radial diffusion while in situ acceleration (violating the first adiabatic invariant) has to be invoked to explain the enhancement of the outer belt electrons during another storm.
DE: 2716 Energetic particles: precipitating
DE: 2720 Energetic particles: trapped
DE: 2730 Magnetosphere: inner
DE: 2774 Radiation belts
DE: 2788 Magnetic storms and substorms (7954)
SC: SPA-Magnetospheric Physics [SM]
MN: 2007 Fall Meeting