An unstable arch model of a solar flare

Physics

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Magnetohydrodynamic Stability, Solar Flares, Solar Magnetic Field, Stellar Models, Electric Current, Electromagnetic Fields, Electrostatics, Magnetic Flux, Shock Waves, Skylab Program, Solar Atmosphere, Solar Corona, Solar Limb

Scientific paper

The theoretical consequences of assuming that a current flows along flaring arches consistent with a twist in the field lines of these arches are examined. It is found that a sequence of magnetohydrodynamic (MHD) and resistive MHD instabilities driven by the assumed current (which we refer to as the toroidal current) can naturally explain most manifestations of a solar flare. The principal flare instability in the proposed model is the resistive kink (or tearing mode in arch geometry) which plays the role of thermalizing some of the field energy in the arch and generating X-configured neutral points needed for particle acceleration. The difference between thermal and nonthermal flares is elucidated and explained, in part, by amplitude-dependent instabilities. The criteria for the generation of flare shocks strongly depend on the magnitude and gradient steepness of the toroidal current, which also are found to determine the volume and rate of energy release.

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