HR: 0800h
AN: P51A-1417    [Abstracts]
TI: New Simulations of Saturn's Polar Wind
AU: * Glocer, A
EM: aglocer@umich.edu
AF: University of Michigan, Space Research Building University of Michigan 2455 Hayward St., Ann Arbor, MI 48109-2143 United States
AU: Gombosi, T
EM: tamas@umich.edu
AF: University of Michigan, Space Research Building University of Michigan 2455 Hayward St., Ann Arbor, MI 48109-2143 United States
AU: Hansen, K
EM: kenhan@umich.edu
AF: University of Michigan, Space Research Building University of Michigan 2455 Hayward St., Ann Arbor, MI 48109-2143 United States
AU: Toth, G
EM: gtoth@umich.edu
AF: University of Michigan, Space Research Building University of Michigan 2455 Hayward St., Ann Arbor, MI 48109-2143 United States
AB: We present preliminary results of a new simulation of Saturn's polar wind. The results include new vertical ion and electron density profiles, fluxes, and net source rates. Our model solves the 13 moment gyrotropic transport equations. The gyration dominated assumption allows us to assume that the flow is field aligned, and justifies the use of a one dimensional model. Furthermore, the effect of solar zenith angle and optical depth on the solar flux is taken into account. While capable of modeling transient behavior, only steady state results are presented. Similarly, the ability to include field aligned currents is built into the model, but their effect is not yet studied. By combining polar wind model output with a global MHD simulation of the magnetosphere-ionosphere system, we are able to calculate the net ionospheric source due to the polar wind. Like Earth, we expect that Saturn's ionosphere is an important source of magnetospheric plasma. The recent arrival of Cassini is giving unprecedented amounts of data. The time is therefore ripe for an attempt to characterize the ionospheric source at Saturn, and this simulation will help further this objective.
DE: 5739 Meteorology (3346)
DE: 6275 Saturn
SC: Planetary Sciences [P]
MN: 2004 AGU Fall Meeting