Astronomy and Astrophysics – Astronomy
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011spd....42.2314m&link_type=abstract
American Astronomical Society, SPD meeting #42, #23.14; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
Flux rope models of coronal mass ejections (CMEs) typically predict the formation of a reconnecting current sheet between the flare site and the rising plasmoid. Sunward outflow is directed towards regions of high plasma and magnetic pressure, whereas antisunward outflow impacts the rising flux rope. There are likely to be strong gradients along the outflow direction for upstream density, pressure, and magnetic field strength. We use resistive magnetohydrodynamic (MHD) simulations to investigate the impact of asymmetry and current sheet motion during the reconnection process in the context of CME current sheets. Simulations of X-line retreat predict that most of the outflow energy is directed upward towards the rising flux rope, and show that the bulk plasma flow at the X-line is sometimes in the opposite direction of X-line retreat. CME current sheets are expected to be unstable to the formation of plasmoids, and our simulations of multiple competing X-lines show that the flow stagnation point is typically located between the X-line and a centrally located plasma pressure maximum. Simulations of line-tied asymmetric inflow reconnection show slow current sheet drifting and skewing of post-flare loops.
Lin Juhn-Jong
Miralles Mari Paz
Murphy Nicholas Arnold
Shen Caiming
Young A. K.
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