Global MHD Modeling of Solar Wind Density Changes

Details Global MHD Modeling of Solar Wind Density Changes Global MHD Modeling of Solar Wind Density Changes

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsm31b0774k&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SM31B-0774

Physics

2753 Numerical Modeling, 2784 Solar Wind/Magnetosphere Interactions

Scientific paper

A sudden increase in the solar wind dynamic pressure compresses the magnetosphere and launches compressional waves into the magnetosphere. Using BATS-R-US, a global 3D MHD model developed by the University of Michigan, we will study the different responses of the magnetosphere to two different solar wind dynamic pressure changes. One case will involve a moderately slow solar wind density step increase. The second case will involve a more rapid solar wind density pulse. The differences in the global response of the magnetosphere, including the ionosphere and the location of the field-aligned current generation, for the two cases will be presented. We will present results on the formation of traveling convection vortices. We will compare the results of the simulation to current theories of field-aligned current generation from dynamic pressure changes.

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