HR: 1340h
AN: SH23A-0325    [Abstracts]
TI: CME-Driven Shocks and Particle Acceleration in Solar Corona and Interplanetary Space
AU: * Zhang, T
EM: zhangt@cspar.uah.edu
AF: Alamama A&M University, Physics Department, Alabama A&M University, Normal, AL 35762
AU: Wu, S
EM: wus@cspar.uah.edu
AF: University of Alabama in Huntsville, Center for Space Plasma and Aeronomic Research, University of Alabama in Huntsville, Huntsville, AL 35899
AU: Tan, A
EM: arjun.tan@email.aamu.edu.
AF: Alamama A&M University, Physics Department, Alabama A&M University, Normal, AL 35762
AU: Fry, C
EM: gfry@expi.com
AF: University of Alabama in Huntsville, Center for Space Plasma and Aeronomic Research, University of Alabama in Huntsville, Huntsville, AL 35899
AU: Fry, C
EM: gfry@expi.com
AF: Exploration Physics International, Inc., Suite 37-105, 6275 University Drive NW, Huntsville, AL 35806
AB: Solar energetic particles (SEPs) that severely affect space weather are understood to come from two different sources: (1) solar flares and (2) coronal mass ejections (CMEs)-driven shocks. The SEPs from solar flares are usually classified as the impulsive events with extreme enhancements in ³He/⁴He and enhanced heavy ions caused by the particle-wave resonances and the first/second-order Fermi acceleration. On the other hand, the most intense SEP (or gradual) events are believed to be produced by the acceleration of CME-driven shocks via the Fermi acceleration mechanism for quasi-parallel shocks and shock-drift acceleration for quasi-perpendicular shocks. By the motions of the CME-driven oblique shocks across the background magnetic field lines, an electric field is induced, which is effective in the acceleration of charged particles. The acceleration process strongly depends on not only the strength of the electric field induced by the across-field line motions, but also on the CME-driven shock geometric configuration, propagation, and temporal and spatial evolutions. In this presentation, we will present our recent simulation results of the CME-driven shock properties and the induced electric field in terms of an azimuthal symmetrical MHD simulation model for both slow (accelerated) and fast (constant speed) CMEs with and without loop structures. We will also analytically estimate the fluxes of energetic particles accelerated by the CME-driven shocks and compare the results with observations.
DE: 2139 Interplanetary shocks
DE: 7509 Corona
DE: 7513 Coronal mass ejections (2101)
DE: 7514 Energetic particles (2114)
DE: 7974 Solar effects
SC: SPA-Solar and Heliospheric Physics [SH]
MN: Fall Meeting 2005