HR: 0830h
AN: SM31C-1123    [PDF]
TI: Asymmetries in the Martian magnetotail plasma as seen in 3D fluid simulations.
AU: * Harnett, E M
EM: eharnett@ess.washington.edu
AF: Department of Earth and Space Science University of Washington, Box 351310, Seattle, WA 98195-1310 United States
AU: Winglee, R M
EM: winglee@ess.washington.edu
AF: Department of Earth and Space Science University of Washington, Box 351310, Seattle, WA 98195-1310 United States
AB: Previous 3D single fluid simulations showed that the strong magnetic anomalies on the Martian surface can lead to the formation of a mini-magnetopause either in place of or in addition to the magnetic pileup boundary. The anomalous magnetic field also leads to asymmetries in the tail plasma that change when the location of the strongest anomalies are rotated off of local noon. 3D multifluid simulations of a magnetize Mars in the solar wind show the relative importance of solar wind and ionospheric ions in the formation of the tail asymmetries and that ionospheric outflow plays a large role in the formation of the asymmetries. Tracking changes in the ionospheric outflow rate for different orientations of the surface magnetic field both relative to the noon meridian and the IMF shows the variation in relative outflow of atomic and molecular oxygen.
DE: 2736 Magnetosphere/ionosphere interactions
DE: 2744 Magnetotail
DE: 2753 Numerical modeling
DE: 2756 Planetary magnetospheres (5443, 5737, 6030)
DE: 6225 Mars
SC: SPA - Magnetospheric Physics [SM]
MN: 2003 Fall Meeting