HR: 10:35h
AN: SH51B-02    [PDF]
TI: The Three Modes of Magnetospheric Behavior Observed During Magnetic Storms
AU: * Clauer, C R
EM: rclauer@umich.edu
AF: University of Michigan, Center for Space Environment Modeling, 2455 Hayward, Ann Arbor, MI 48109-2143 United States
AU: Kozyra, J U
EM: jukozyra@umich.edu
AF: University of Michigan, Center for Space Environment Modeling, 2455 Hayward, Ann Arbor, MI 48109-2143 United States
AU: DeJong, A
EM: dejonga@umich.edu
AF: University of Michigan, Center for Space Environment Modeling, 2455 Hayward, Ann Arbor, MI 48109-2143 United States
AU: Cai, X
EM: xcai@umich.edu
AF: University of Michigan, Center for Space Environment Modeling, 2455 Hayward, Ann Arbor, MI 48109-2143 United States
AU: Welling, D
EM: dwelling@umich.edu
AF: University of Michigan, Center for Space Environment Modeling, 2455 Hayward, Ann Arbor, MI 48109-2143 United States
AU: Liemohn, M W
EM: liemohn@umich.edu
AF: University of Michigan, Center for Space Environment Modeling, 2455 Hayward, Ann Arbor, MI 48109-2143 United States
AU: Borovsky, J E
EM: borovsky@nisdp0.lanl.gov
AF: Los Alamos National Laboratory, Space & Atmospheric Science Group,, Los Alamos, NM 87545 United States
AB: Understanding geomagnetic storms is a paramount space weather problem as well as a fundamental scientific challenge. The processes that operate during magnetic storms have been areas of active investigation and significant discussion for many years. We believe that it is possible now to identify three distinct modes of magnetospheric operation during various geomagnetic storms. One mode consists of periods of enhanced steady magnetospheric convection (SMC) punctuated by isolated magnetospheric substorm expansions. A second mode of operation consists of periodic substorm expansions. The third mode of operation is characterized by global sawtooth oscillations in the magnetic field tilt and particle fluxes measured at geostationary orbit. We will report on the means to identiry and distinguish these three modes of operation. The conditions under which each mode appears to become dominant during a particular storm appears to lie both in the solar wind driving conditions as well as in some internal magnetospheric conditions.
DE: 2740 Magnetospheric configuration and dynamics
DE: 2760 Plasma convection
DE: 2778 Ring current
DE: 2784 Solar wind/magnetosphere interactions
DE: 2788 Storms and substorms
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting