Energy release in solar flares

Details Energy release in solar flares Energy release in solar flares

Sep 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984soph...94..341s&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 94, Sept. 1984, p. 341-357.

Physics

105

Energy Dissipation, Magnetic Field Configurations, Solar Flares, Solar Magnetic Field, Millimeter Waves, Photosphere, Solar Corona, Solar Prominences, Solar X-Rays

Scientific paper

On the basis of observations of energy release in solar flares, it is proposed that different processes may operate on four different time scales; (1) the subsecond scale of subbursts that prominently figure in mm-wave records; (2) the few-seconds scale of elementary bursts featured in hard X-ray records; (3) the few-minutes scale of the impulsive phase; and (4) the longer than tens-of-minutes scale of the gradual phase. It is proposed that the magnetic field concentration into 'magnetic knots' at the photosphere is of consequence to coronal magnetic field structure, so that magnetic fields in this region may be seen as an array of elementary flux tubes. It is further proposed that the gradual phase of energy release involves a steady process of reconnection, while the impulsive phase involves a more stochastic process of reconnection due to mode interaction.

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