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paty

HR: 0830h
AN: SM21A-0527
TI: Multi-Fluid Simulations of the Jovian Magnetosphere
AU: * Paty, C S
EM: carol@ess.washington.edu
AF: University of Washington Department of Earth and Space Sciences, Box 351310, Seattle, WA 98195-1310 United States
AU: Winglee, R M
EM: winglee@ess.washington.edu
AF: University of Washington Department of Earth and Space Sciences, Box 351310, Seattle, WA 98195-1310 United States
AU: Harnett, E M
EM: eharnett@ess.washington.edu
AF: University of Washington Department of Earth and Space Sciences, Box 351310, Seattle, WA 98195-1310 United States
AB: The dynamics of the Jovian magnetosphere are controlled by three sources; the solar wind, the Jovian ionosphere, and the Jovian moons. The system is substantially modified from the terrestrial magnetosphere because the rapid rotation of Jupiter produces strong acceleration of heavy ion species such as O+ and S+ emanating form the Jovian moons. Because of this acceleration these heavy ions can dominate the energy and momentum transport within at least the inner magnetosphere and possibly much of the outer magnetosphere. Multi-fluid simulations are used to model the acceleration of Jovian heavy ions and their effect on the overall shape on the Jovian magnetosphere. We show how the presence of heavy ions enhances the equatorial current sheet, which modifies the overall shape of the magnetosphere. In addition, they produce local inhomogeneities in the velocity field that leads to locally enhanced field-aligned currents and accelerated particle populations. The mixing of these accelerated heavy ions with the solar wind plasma leads to distinct particle populations in the Jovian magnetosphere.
DE: 2708 Current systems (2409)
DE: 5737 Magnetospheres (2756)
DE: 6220 Jupiter
DE: 7807 Charged particle motion and acceleration
DE: 7827 Kinetic and MHD theory
SC: SPA: Magnetospheric Physics [SM]
MN: 2002 Fall Meeting