Interplanetary Shock Interaction with the Magnetosphere: Model Results

Details Interplanetary Shock Interaction with the Magnetosphere: Model Results Interplanetary Shock Interaction with the Magnetosphere: Model Results

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsm31a1202s&link_type=abstract

American Geophysical Union, Fall Meeting 2004, abstract #SM31A-1202

Physics

Plasma Physics

2724 Magnetopause, Cusp, And Boundary Layers, 2728 Magnetosheath, 2753 Numerical Modeling, 2784 Solar Wind/Magnetosphere Interactions

Scientific paper

The interaction of an abrupt change in the solar wind dynamic pressure with the magnetosphere is one of the fundamental problems in space plasma physics. We employ the Bats-R-Us model with high temporal (20 s) and spatial (0.125 RE maximum) resolution to address this problem. The interaction of the interplanetary shock with the bow shock causes the latter to begin moving inward and launches a fast mode wave into the magnetosheath. The fast mode wave keeps pace with the interplanetary shock in the plane containing the interplanetary magnetic field (IMF), but moves ahead in the plane perpenedicular to the (northward) IMF. The interaction of the transmitted shock with the magnetopause causes the latter boundary to move inward and launches a fast mode wave into the magnetosphere. The fast mode wave is reflected at the plasmapause. The reflected wave further enhances outer magnetospheric magnetic field strengths, causes the magnetopause to move back outward, and is transmitted into the magnetosheath. When it reaches the bow shock it causes that boundary to move back outward also. Both the magnetopause and the bow shock move inward and outward smoothly during the entire process via a nearly global breathing mode. No large amplitude boundary waves are generated. For discontinuities oriented along the spiral IMF, the boundary motion spreads both dawnward and duskward from an initial location at post-noon local times.

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