Physics
Scientific paper
Mar 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986soph..104....1p&link_type=abstract
(CNR, Workshop on Radio Continua during Solar Flares, Duino, Italy, May 27-31, 1985) Solar Physics (ISSN 0038-0938), vol. 104, M
Physics
22
Magnetohydrodynamic Stability, Solar Flares, Energy Dissipation, Particle Acceleration, Solar Magnetic Field, Sunspots, Tearing Modes (Plasmas), Temporal Distribution
Scientific paper
Our current understanding of the MHD of the flare process is summarised, with some emphasis on processes which produce strong impulsive electric fields and current filamentation. As an introduction, a description of the two main types of flare (i.e, simple-loop and two-ribbon) is given, together with an account of the two branches of reconnection theory (tearing modes and the Petschek-Sonnerup mechanism). Modern numerical experiments of reconnection suggest impulsive bursty acceleration of particles in many small regions of width a hundred kilometers or less. This is followed by a discussion of the eruptive instability thought to initiate a large flare and of the reconnection process of energy release. Finally, the role of emerging flux and horizontally moving satellite sunspots is discussed briefly.
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