Solar Wind Driven Auroral Wind, with Global Consequences

Details Solar Wind Driven Auroral Wind, with Global Consequences Solar Wind Driven Auroral Wind, with Global Consequences

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufmsm34a..07m&link_type=abstract

American Geophysical Union, Fall Meeting 2005, abstract #SM34A-07

Physics

2431 Ionosphere/Magnetosphere Interactions (2736), 2784 Solar Wind/Magnetosphere Interactions

Scientific paper

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.

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