Solar wind plasma controlling magnetospheric coupling efficiency

Details Solar wind plasma controlling magnetospheric coupling efficiency Solar wind plasma controlling magnetospheric coupling efficiency

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsm31c..05p&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SM31C-05

Physics

2724 Magnetopause And Boundary Layers, 2731 Magnetosphere: Outer, 2753 Numerical Modeling, 2784 Solar Wind/Magnetosphere Interactions

Scientific paper

A wealth of new observational evidence add to the earlier understanding of solar wind - magnetosphere coupling the importance of solar wind speed and density. Statistical analysis shows that for the same electric field, events with higher solar wind speed cause larger AE disturbance than those with lower speed and higher magnetic field. Analysis of abrupt solar wind density changes shows that the ionospheric activity is lower for lower values of the density, and that the response is near-simultaneous with the arrival of the front at the magnetopause. Global MHD simulations confirm these results: The reconnection efficiency at the magnetopause is a strong function of the solar wind speed, and responds to a lesser extent also to changes in the solar wind density. Furthermore, series of simulation runs confirm the higher activity during higher solar wind speed, and the role of dynamic pressure in driving the magnetotail activity. Lastly, both observational and simulation evidence suggest that the coupling efficiency is higher for lower level of solar wind driving such that a smaller percentage of incident energy is processed in the magnetotail and auroral ionosphere during strong magnetic activity. Here we use both observational and simulation results to extract the processes via which the solar wind plasma parameters affect the level of activity both in the magnetotail and in the auroral ionosphere.

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