Three-dimensional MHD instability of spontaneous fast magnetic reconnection in geomagnetotail

Details Three-dimensional MHD instability of spontaneous fast magnetic reconnection in geomagnetotail Three-dimensional MHD instability of spontaneous fast magnetic reconnection in geomagnetotail

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsm51c1827s&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SM51C-1827

Physics

[2723] Magnetospheric Physics / Magnetic Reconnection

Scientific paper

In recent multi-satellite observations such as THEMIS, various plasma dynamics related to the fast magnetic reconnection in geomagnetotail is actively studied. However, the three-dimensional structure of the fast magnetic reconnection itself is still unclear. According to our previous MHD studies, it has been revealed that two-dimensional spontaneous fast magnetic reconnection which can be quasi-steady state is unstable in three-dimensional perturbation, resulting in intermittent and unsteady three-dimensional fast magnetic reconnection even in one-dimensional current sheet. Those studies were successfully applied for solar flare observations such as TRACE EUV image data and, now, is tried to be applied for the geomagnetotail dynamics. In geomagnetotail, since the current sheet has a three-dimensional structure and may be disturbed by various geomagnetosphere’s three-dimensional plasma convections, the three-dimensional instability of fast magnetic reconnection process may be largely modified from the ideal and simple geometry models. In this study, using global three-dimensional MHD simulation including various interactions between solar winds and geomagnetosphere, it is visually shown that how the three-dimensional spontaneous fast magnetic reconnection is caused in geomagnetotail.

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