MHD Simulation of Solar Wind Dynamic Pressure Changes

Details MHD Simulation of Solar Wind Dynamic Pressure Changes MHD Simulation of Solar Wind Dynamic Pressure Changes

May 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsh52a..23k&link_type=abstract

American Geophysical Union, Spring Meeting 2002, abstract #SH52A-23

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 three different solar wind dynamic pressure changes. One case will involve a slow solar wind density step increase. The second case will involve a more rapid step increase. The third case will be a solar wind density pulse. The differences in the global responses of the magnetosphere for the three cases will be presented. In particular, we will look at the differences in the responses of the ionosphere for the step increase and the pulse. We will compare the results of the simulation to current theories of field-aligned current generation from dynamic pressure changes.

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