Activation of solar flares

Details Activation of solar flares Activation of solar flares

Nov 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984esasp.207...57c&link_type=abstract

In ESA Plasma Astrophys. p 57-63 (SEE N85-22270 12-90)

Physics

1

Magnetohydrodynamic Stability, Solar Corona, Solar Flares, Solar Magnetic Field, Magnetohydrodynamic Shear Heating, Plasma Equilibrium, Pressure Gradients, Solar Activity Effects

Scientific paper

The physics of the activation of two-ribbon solar flares via the MHD instability of coronal arcades is presented. The destabilization of a preflare magnetic field is necessary in order for a rapid energy release, characteristic of the impulsive phase of the flare, to occur. The authors examine the stability of a number of configurations and discuss the physical consequences and relative importance of varying pressure profiles and different sets of boundary conditions (involving field-line tying). Interchange modes, driven unstable by pressure gradients, are candidates for instability. Shearless vs. sheared equilibria are also discussed.

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