HR: 17:30h
AN: SM34A-07    [Abstracts]
TI: Solar Wind Driven Auroral Wind, with Global Consequences
AU: * Moore, T E
EM: thomas.e.moore@nasa.gov
AF: NASA's Goddard Space Flight Center, Laboratory for Solar and Space Physics, Greenbelt, MD 20771 United States
AU: Fok, M H
EM: mei-ching.fok@nasa.gov
AF: NASA's Goddard Space Flight Center, Laboratory for Solar and Space Physics, Greenbelt, MD 20771 United States
AU: Delcourt, D C
EM: dominique.delcourt@cetp.ipsl.fr
AF: CETP, 4, Ave de Neptune, Saint Maur, TX 94107 France
AU: Slinker, S J
EM: slinker@ppdu.nrl.navy.mil
AF: Naval Research Laboratory, 4555 Overlook Ave., SW, Washington, DC 20375 United States
AU: Fedder, J A
EM: fedder@ppdu.nrl.navy.mil
AF: LET Corporation, 4431 MacArthur Blvd. N.W., Washington, DC 20007 United States
AU: Buenfil, M J
EM: manuel.buenfil@nasa.gov
AF: NASA's Goddard Space Flight Center, Laboratory for Solar and Space Physics, Greenbelt, MD 20771 United States
AB: We investigate the detailed local structure of auroral wind outflows produced by prototypical solar wind disturbances of interplanetary magnetic field and the plasma dynamic pressure. Further, we track the global circulation and energization of auroral wind plasmas throughout the magnetosphere through precipitation or escape into the downstream solar wind. We use the full equations of motion of solar wind and auroral wind ions within fields produced by a global MHD simulation of the dynamic solar wind interaction. We use the dynamic hot plasma density and Poynting energy flux specified at the inner boundary of the MHD simulation as drivers of ion outflow fluxes using local empirical relations obtained from the FAST and Polar missions. Birkeland currents are used to derive a field-parallel potential drop from a Knight-like relation [as modified by Lyons and Evans, 1980]. This potential drop is applied to each ion as an initial bulk energy, and added to a thermal energy driven by the locally incident Poynting flux. The solar wind pressure increase case (Bz=0) produces an immediate substorm, while the SBz interval (embedded in NBz) produces a substorm after about one hour of development. Both disturbances enhance the auroral wind flux and heavy ion pressure of the magnetosphere substantially, with complex dynamic structuring by auroral acceleration vortexes and magnetotail reconnection. Comparisons are made with observations during disturbed periods.
UR: http://hpb.gsfc.nasa.gov/public/traj/dynamic-fields/
DE: 2431 Ionosphere/magnetosphere interactions (2736)
DE: 2784 Solar wind/magnetosphere interactions
SC: SPA-Magnetospheric Physics [SM]
MN: Fall Meeting 2005