HR: 1340h
AN: SM33A-1251    [Abstracts]
TI: Plasma sources and lifetimes within the Jovian magnetosphere
AU: * Stickle, A
EM: astickle@u.washington.edu
AF: University of Washington, Department of Earth and Space Sciences, 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, Seattle, WA 98195-1310 United States
AU: Harnett, E
EM: eharnett@ess.wwashington.edu
AF: University of Washington, Department of Earth and Space Sciences, Seattle, WA 98195-1310 United States
AU: Paty, C
EM: carol@ess.washington.edu
AF: University of Washington, Department of Earth and Space Sciences, Seattle, WA 98195-1310 United States
AB: The Jovian magnetosphere is fed by plasma from Io, the icy Galilean moons and the Jovian ionosphere. The plasmas from these different sources not only differ in mass composition and outflow rate, but also have access to different regions. The mixing of these plasmas plays a critical role in determining the overall size and structure of the Jovian magnetosphere. 3-D multi-fluid simulations that incorporate the heavy and light ion interactions are used to model the mixing of heavy ion torus plasma with light ion outflow from the Jovian magnetosphere. It is shown that at radii smaller than the Io torus the plasma is completely co-rotational and that the main loss mechanism is to the Jovian ionosphere. Light ions continue to have essentially no departure from being fully co-rotational out to about 13 R$_J$, while the heavy torus ions show some slippage with lifetimes of the order of about 60 hrs. Between 13 $R_J$ and about 20 $R_J$ lifetimes of both light and heavy ions is of the order of about 100 hrs. These characteristics are most strongly dependent of the torus plasma density rather than the ionospheric outflow rate. Beyond this distance, deviations from co-rotation becoming an increasing larger effect and lifetimes decrease. The properties of the ionospheric outflows play an increasingly important role in this region. The co-rotation boundary and position of the magnetosphere are shown to move significantly under the convection of torus and ionospheric plasma from the inner magnetosphere into the outer magnetosphere.
DE: 2431 Ionosphere/magnetosphere interactions (2736)
DE: 2463 Plasma convection
DE: 2736 Magnetosphere/ionosphere interactions
DE: 2753 Numerical modeling
SC: SPA-Magnetospheric Physics [SM]
MN: 2004 AGU Fall Meeting