Non-steady Reconnection in Global Simulations of Magnetosphere Dynamics.

Details Non-steady Reconnection in Global Simulations of Magnetosphere Dynamics. Non-steady Reconnection in Global Simulations of Magnetosphere Dynamics.

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsm23c..04k&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SM23C-04

Other

2723 Magnetic Reconnection (7526, 7835), 2740 Magnetospheric Configuration And Dynamics, 2784 Solar Wind/Magnetosphere Interactions, 2788 Magnetic Storms And Substorms (7954), 7526 Magnetic Reconnection (2723, 7835)

Scientific paper

To analyze the non-steady magnetic reconnection during quasi-steady solar wind driving we employed high resolution global MHD model BATSRUS with non-MHD corrections in diffusion regions around the reconnection sites. To clarify the role of small-scale non-MHD effects on the global magnetospheric dynamic we performed simulations with different models of dissipation. We found that magnetopause surface is not in steady state even during extended periods of steady solar wind conditions. The so-called tilted reconnection lines become unstable due to formation of pressure bubbles, strong core field flux tubes, vortices, and traveling magnetic field cavities. Non-steady dayside reconnection results in formation of flux tubes with bended axis magnetically connecting magnetic field cavities generated at flanks and strong core segments formed near the subsolar region. We found that the rate of magnetic flux loading to the tail lobes is not very sensitive to the dissipation mechanism and details of the dayside reconnection. On the other hand the magnetotail reconnection rate, the speed of the reconnection site retreat and the global magnetotail dynamics strongly depend on the model of dissipation. THEMIS and Cluster observations are consistent with signatures predicted by simulations.

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