HR: 0830h
AN: SM51B-0525    [PDF]
TI: Modeling relativistic electron fluxes in the inner magnetosphere with spatially distributed models
AU: * Vassiliadis, D
EM: vassi@electra.gsfc.nasa.gov
AF: USRA, NASA/GSFC, Code 692, Greenbelt, MD 20771 United States
AU: Fung, S F
EM: fung@mail630.gsfc.nasa.gov
AF: NASA/GSFC, Code 630, Greenbelt, MD 20771 United States
AU: Klimas, A J
EM: alex.klimas@nasa.gov
AF: NASA/GSFC, Code 692, Greenbelt, MD 20771 United States
AU: Shao, X
EM: shao@mail630.gsfc.nasa.gov
AF: NRC, NASA/GSFC, Code 630, Greenbelt, MD 20771 United States
AU: Baker, D N
EM: daniel.baker@lasp.colorado.edu
AF: LASP, University of Colorado, Boulder, CO 80309 United States
AU: Kanekal, S G
EM: kanekal@surya.umd.edu
AF: Catholic University of America, Department of Physics, Washington, DC 20007 United States
AU: Weigel, R S
EM: robert.weigel@lasp.colorado.edu
AF: LASP, University of Colorado, Boulder, CO 80309 United States
AU: Rigler, E J
EM: jrigler@colorado.edu
AF: LASP, University of Colorado, Boulder, CO 80309 United States
AB: The spatial and temporal dynamics of relativistic electron fluxes are modeled using ARMA-type filters parametrized by L shell in the range 1-10. The filter coefficients are qualitatively different for the 3 regions Pi that make up the range L$>3$. Region P0, as well as the slot, are related to a rapid response ($<1$ day) to ejecta and clouds, and diffusive dynamics. Region P1 is related to the 2-3 day response to speed variations, such as those of high-speed streams, while region P2 responds to Northward Bz. The fluxes in both regions exhibit diffusive as well as convective dynamics. The filter approach is used to produce effective diffusion coefficients for the flux, and, for P1 and P2, a range of convection speed as functions of L. The predictive capability of these regional models is estimated.
DE: 2720 Energetic particles, trapped
DE: 2730 Magnetosphere--inner
SC: SPA - Magnetospheric Physics [SM]
MN: 2003 Fall Meeting