Multiscale Modeling of Solar Coronal Magnetic Reconnection

Details Multiscale Modeling of Solar Coronal Magnetic Reconnection Multiscale Modeling of Solar Coronal Magnetic Reconnection

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsm31b1873a&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SM31B-1873

Physics

Plasma Physics

[7513] Solar Physics, Astrophysics, And Astronomy / Coronal Mass Ejections, [7827] Space Plasma Physics / Kinetic And Mhd Theory, [7835] Space Plasma Physics / Magnetic Reconnection

Scientific paper

Magnetic reconnection is widely believed to be the primary process by which the magnetic field releases energy to plasma in the Sun's corona. For example, in the breakout model for the initiation of coronal mass ejections/eruptive flares, reconnection is responsible for the catastrophic destabilizing of magnetic force balance in the corona, leading to explosive energy release. A critical requirement for the reconnection is that it have a "switch-on' nature in that the reconnection stays off until a large store of magnetic free energy has built up, and then it turn on abruptly and stay on until most of this free energy has been released. We discuss the implications of this requirement for reconnection in the context of the breakout model for CMEs/flares. We argue that it imposes stringent constraints on the properties of the flux breaking mechanism, which is expected to operate in the corona on kinetic scales. We present numerical simulations demonstrating how the reconnection and the eruption depend on the effective resistivity, i.e., the effective Lundquist number, and propose a model for incorporating kinetic flux-breaking mechanisms into MHD calculation of CMEs/flares. This work has been supported by the NASA HTP, SR&T, and LWS programs. High-resolution simulation of a breakout CME showing details of the reconnection region (Karpen et al 2010).

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