Simulations of Flare Reconnection in Breakout Coronal Mass Ejections

Details Simulations of Flare Reconnection in Breakout Coronal Mass Ejections Simulations of Flare Reconnection in Breakout Coronal Mass Ejections

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009spd....40.2007d&link_type=abstract

American Astronomical Society, SPD meeting #40, #20.07; Bulletin of the American Astronomical Society, Vol. 41, p.853

Astronomy and Astrophysics

Astronomy

Scientific paper

We report 3D MHD simulations of the flare reconnection in the corona below breakout coronal mass ejections (CMEs). The initial setup is a single bipolar active region imbedded in the global-scale background dipolar field of the Sun, forming a quadrupolar magnetic configuration with a coronal null point. Rotational motions applied to the active-region polarities at the base of the atmosphere introduce shear across the polarity inversion line (PIL). Eventually, the magnetic stress and energy reach the critical threshold for runaway breakout reconnection, at which point the sheared core field erupts outward at high speed. The vertical current sheet formed by the stretching of the departing sheared field suffers reconnection that reforms the initial low-lying arcade across the PIL, i.e., creates the flare loops. Our simulation model, the Adaptively Refined MHD Solver, exploits local grid refinement to resolve the detailed structure and evolution of the highly dynamic current sheet. We are analyzing the numerical experiments to identify and interpret observable signatures of the flare reconnection associated with CMEs, e.g., the flare loops and ribbons, coronal jets and shock waves, and possible origins of solar energetic particles.
This research was supported by NASA and ONR.

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