Modeling Free Energy & Reconnection in the Corona

Details Modeling Free Energy & Reconnection in the Corona Modeling Free Energy & Reconnection in the Corona

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006spd....37.0908w&link_type=abstract

American Astronomical Society, SPD meeting #37, #9.08; Bulletin of the American Astronomical Society, Vol. 38, p.237

Computer Science

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Scientific paper

The injection and storage of magnetic free energy into the coronal magnetic field is an essential component of the widely accepted ``storage & release'' paradigm of solar flares and CMEs.A central role in many models of both the storage and release phases is played by magnetic reconnection --- which can form an unstable structure (e.g., by flux cancellation) and/or reduce confinement allowing a metastable structure to erupt (as in the breakout model).To investigate changes in magnetic energy and field line connectivity in the presence of shearing, convergence, and flux cancellation, we have used the ARMS code, a 3-D, flux-corrected transport MHD code with adaptive mesh refinement, to simulate the evolution of coronal magnetic fields driven by prescribed photospheric motions.Here, we present the preliminary results of our investigations, and outline directions for future studies.This work was supported by ONR, NASA's SEC Theory program, and by a grant of computer time from the DOD High Performance Computing Modernization Program.

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