Activation of Solar Flares
Abstract
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.
- Publication:
-
Plasma Astrophysics
- Pub Date:
- November 1984
- Bibcode:
- 1984ESASP.207...57C
- Keywords:
-
- Magnetohydrodynamic Stability;
- Solar Corona;
- Solar Flares;
- Solar Magnetic Field;
- Magnetohydrodynamic Shear Heating;
- Plasma Equilibrium;
- Pressure Gradients;
- Solar Activity Effects;
- Solar Physics