Tail Current Sheet Under Strong Driving: MHD Simulations and in-situ Observations Compared

Details Tail Current Sheet Under Strong Driving: MHD Simulations and in-situ Observations Compared Tail Current Sheet Under Strong Driving: MHD Simulations and in-situ Observations Compared

May 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agusmsm44a..04p&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SM44A-04

Physics

2740 Magnetospheric Configuration And Dynamics, 2744 Magnetotail, 2753 Numerical Modeling, 2760 Plasma Convection (2463)

Scientific paper

We use in-situ multipoint measurements and global MHD simulations to examine the large-scale structure of the tail current sheet and its response to the variable solar wind driving. The Lyon - Fedder - Mobarry code was run for three events: A substorm on Aug 11, 2002, a steady convection event on Feb 4, 1998, and a sawtooth event on Apr 18, 2002. For each of the events, multispacecraft observations in the inner and mid-magnetotail reveal the timing, location, and structure of an intense current sheet that developed in the tail. Each of the events was driven by an extended period of southward IMF, but the dynamics were quite different: During the substorm, gradual intensification and thinning of the current sheet led to the substorm onset after about 1 hour of growth phase. The SMC period was characterized by a relatively intense current sheet that remained stable over a period of almost 9 hours. The sawtooth events show repeated injections, which disrupt part, but not all, of the current in the inner magnetosphere. We use the MHD simulations to quantify the magnetospheric response to the solar wind driving and to seek for dynamic elements in the global system that control the large-scale response of the magnetotail.

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