HR: 0800h
AN: SH51A-0267    [Abstracts]
TI: Solar Energetic Particles Acceleration and Transport Model Coupled With a Realistic CME Model.
AU: * Sokolov, I V
EM: igorsok@umich.edu
AF: Center for Space Environment Modeling, University of Michigan, 2455 Hayward Str, Ann Arbor, MI 48109
AU: Roussev, I I
EM: iroussev@umich.edu
AF: Center for Space Environment Modeling, University of Michigan, 2455 Hayward Str, Ann Arbor, MI 48109
AU: Kota, J
EM: kota@LPL.Arizona.EDU
AF: Planetary Laboratory, University of Arizona, Tucson, Az 85721
AU: Gombosi, T I
EM: tamas@umich.edu
AF: Center for Space Environment Modeling, University of Michigan, 2455 Hayward Str, Ann Arbor, MI 48109
AU: Manchester, W B
EM: chipm@umich.edu
AF: Center for Space Environment Modeling, University of Michigan, 2455 Hayward Str, Ann Arbor, MI 48109
AB: Solar Energetic Particles (SEPs) accelerated during and after a Coronal Mass Ejection (CME) produce radiation hazards on board manned and unmanned spacecraft that are not shielded by the Earth's magnetic field. To investigate the particle acceleration by the shock wave which arises from the CME and a subsequent SEPs transport in the realistic magnetic field, a realistic magnetic field near the Sun and in the inner heliosphere should be taken into account. To achieve this, we coupled the available MHD model for CME, which is based on the BATSRUS code, to the kinetic code for SEP using Field-Line-Advection Model for a Particle Acceleration (FLAMPA). The FLAMPA assumes coronal and interplanenetary magnetic fields to be ideally frozen into a moving plasma and neglects the cross-field particle diffusion, however it involves the first order Fermi acceleration, particle adiabatic focusing and SEP scattering by a hydromagnetic turbulence. In this presentation we compare the SEP flux at 1 AU obtained with two alternative models for CME dynamics (using the Gibson-Low model or applying a slow sheared plasma motion to create a flux rope) and with two SEP models (averaged or not averaged by the particle pitch-angle). Comparing with the data observed at 1 AU after the 1998 May,2 event, we validate the models. The SEP acceleration in repetitive CME events will be provided too.
DE: 7514 Energetic particles (2114)
DE: 7524 Magnetic fields
DE: 2114 Energetic particles, heliospheric (7514)
DE: 2139 Interplanetary shocks
DE: 2149 MHD waves and turbulence
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2004 AGU Fall Meeting