HR: 1330h
AN: SH42A-0484    [PDF]
TI: Entry and Acceleration of Solar Wind Electrons in the Earth's Outer Magnetosphere
AU: * Schriver, D
EM: dave@igpp.ucla.edu
AF: IGPP/UCLA, 3860 Slichter Hall, Los Angeles, CA 90095-1567 United States
AU: Ashour-Abdalla, M
EM: mabdalla@igpp.ucla.edu
AF: IGPP/UCLA, 3860 Slichter Hall, Los Angeles, CA 90095-1567 United States
AU: Zelenyi, L
EM: lzelenyi@iki.rssi.ru
AF: Russian Academy of Science, Space Research Institute, Moscow GSP-7, 117997 Russian Federation
AU: Gombosi, T
EM: tamas@umich.edu
AF: University of Michigan, Space Physics Research Laboratory, Ann Arbor, MI 48109-2143 United States
AU: Ridley, A
EM: ridley@umich.edu
AF: University of Michigan, Space Physics Research Laboratory, Ann Arbor, MI 48109-2143 United States
AU: De Zeeuw, D
EM: darrens@umich.edu
AF: University of Michigan, Space Physics Research Laboratory, Ann Arbor, MI 48109-2143 United States
AU: Toth, G
EM: gtoth@umich.edu
AF: University of Michigan, Space Physics Research Laboratory, Ann Arbor, MI 48109-2143 United States
AU: Monostori, G
EM: gmonostori@umich.edu
AF: Eotvos University, Physics Department, Budapest, 11665 Hungary
AB: It is well known that during the recovery of magnetic storms, relativistic electron fluxes are usually enhanced over pre-storm values in the inner magnetosphere near geosynchronous orbit. Although the final acceleration of electrons to MeV energies most likely occurs in the inner magnetosphere, observations indicate that an enhanced flux of energized electrons ($>$ 10 keV) forms in the so-called seed region located at about 10 RE radially from the Earth in the equatorial plane. To examine the acceleration of electrons from the solar wind to the seed region, a study is being undertaken whereby electron trajectories are followed starting upstream of the bow shock, through the magnetopause and throughout the outer magnetosphere. The entry locations of electrons will be examined along with acceleration mechanisms that occur between the solar wind and seed region. The electron particle trajectories are followed based on the guiding center approximation in a global MHD model of the solar wind interaction with the Earth's magnetosphere for various interplanetary magnetic field (IMF) conditions.
DE: 2100 INTERPLANETARY PHYSICS
DE: 2400 IONOSPHERE
DE: 2700 MAGNETOSPHERIC PHYSICS
DE: 7500 SOLAR PHYSICS, ASTROPHYSICS, AND ASTRONOMY
DE: 7800 SPACE PLASMA PHYSICS
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting