HR: 1330h
AN: SH42A-0485    [PDF]
TI: Solar Energetic Ion Entry into the Magnetosphere during a Magnetic Storm
AU: * Richard, R L
EM: rrichard@igpp.ucla.edu
AF: University of California at Los Angeles, Institute of Geophysics and Planetary Physics, 405 Hilgard Ave., Los Angeles, CA 90095-1567 United States
AU: El-Alaoui, M
EM: mostafa@igpp.ucla.edu
AF: University of California at Los Angeles, Institute of Geophysics and Planetary Physics, 405 Hilgard Ave., Los Angeles, CA 90095-1567 United States
AU: Ashour-Abdalla, M
EM: mabdalla@igpp.ucla.edu
AF: University of California at Los Angeles, Institute of Geophysics and Planetary Physics, 405 Hilgard Ave., Los Angeles, CA 90095-1567 United States
AU: Walker, R J
EM: rwalker@igpp.ucla.edu
AF: University of California at Los Angeles, Institute of Geophysics and Planetary Physics, 405 Hilgard Ave., Los Angeles, CA 90095-1567 United States
AB: The magnetic storm of November 24, 2001 was characterized by an increase in the energetic ion flux in the solar wind by more than an order of magnitude over a wide energy range. Following the increase in energetic ions in the solar wind, large increases in ion flux were observed by geosynchronous spacecraft, which was followed later by a substantial drop in DST. In addition, the dynamic pressure increased and the interplanetary magnetic field (IMF), particularly the y component, also increased in magnitude at about the same time as the geosynchronous spacecraft ion flux increased. The question we will address is how the upstream energetic ions contribute to the magnetic storm process and how their transport into the magnetosphere is determined by the magnetospheric configuration. The approach we use is to perform particle tracing calculations in the electric and magnetic fields from a global magnetohydrodynamic (MHD) simulation. We first performed an MHD simulation of this storm interval by using solar wind and IMF time series measured by upstream spacecraft which determine the upstream boundary conditions for the MHD simulation. Then we launched large number of test ions in the time-dependent electric and magnetic fields from the MHD simulation. The accessibility of magnetospheric regions to these ions as well as precipitation and trapping in the model will then be assessed. The flux of energetic particles from the calculations will be compared to the geosynchronous observations.
DE: 2716 Energetic particles, precipitating
DE: 2720 Energetic particles, trapped
DE: 7807 Charged particle motion and acceleration
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting