Magnetic equilibria and instabilities

Details Magnetic equilibria and instabilities Magnetic equilibria and instabilities

Mar 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989soph..121..347s&link_type=abstract

(IAU, Colloquium on Solar and Stellar Flares, 104th, Stanford, CA, Aug. 15-19, 1988) Solar Physics (ISSN 0038-0938), vol. 121, n

Physics

18

Energy Transfer, Magnetohydrodynamic Stability, Solar Flares, Solar Physics, Coronal Loops, Metastable State

Scientific paper

Solar flares are understood as a process of explosive liberation of magnetic energy, coming after a slow phase of energy build-up. The slow evolution of magnetic equilibria may end up with (1) the termination of an equilibrium sequence or (2) an instability. The distinction between the two can be made by drawing schematic potential curves. Case (1) has been extensively studied in two-dimensinal models. The appearance of multiple solutions, or disappearance of a solution takes place as the system evolves away from the current-free configuration. Case (2) can be discussed in terms of ideal MHD or resistive MHD instabilities. A possible route to explosive energy release is suggested by combining these two cases.

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