HR: 1330h
AN: SH42A-0487    [PDF]
TI: Diffusion of Radiation Belt Electrons in Three Dimensions
AU: * Perry, K L
EM: kara.perry@dartmouth.edu
AF: Dartmouth College, Dept of Physics and Astronomy 6127 Wilder Laboratory, Hanover, NH 03755 United States
AU: Hudson, M K
EM: maryk@gaia.dartmouth.edu
AF: Dartmouth College, Dept of Physics and Astronomy 6127 Wilder Laboratory, Hanover, NH 03755 United States
AB: The three dimensional dynamics of relativistic electrons are simulated using guiding center approximation equations to track the bounce and drift motion of particles. The effects of energy, latitude, L value and magnetic field configuration on diffusion rates are examined. Three different dynamic field configurations will be compared. One field model is an analytic model based on a compressed dipole magnetosphere with modeled poloidal mode ULF wave oscillations, including time-varying magnetic and electric field components. The second model developed by Proehl et al. [2002] employs a self-consistent MHD code in dipole geometry driven by a single frequency sinusoidal perturbation at the magnetopause. We have added a solar wind compression of the dipole magnetic field. The third model employs the Lyon-Fedder-Mobary (LFM) 3D MHD code which uses solar wind data at the upstream boundary as input. Comparisons between models and observations of the effects of Ultra Low Frequency (below 10 mHz) wave fields on radial transport and energization of radiation belt electrons will be presented. Proehl, J. A., W. Lotko, I. Kouznetsov and S. D. Geimer, Ultralow-frequency magnetohydrodynamcis in boundary-constrained geomagnetic flux coordinates, J. Geophys. Res., 107, 1225, 2002.
DE: 2720 Energetic particles, trapped
DE: 2753 Numerical modeling
DE: 7807 Charged particle motion and acceleration
DE: 7867 Wave/particle interactions
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting