Prominences and flares

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Aug 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990azh....67..887a&link_type=abstract

Astronomicheskii Zhurnal (ISSN 0004-6299), vol. 67, July-Aug. 1990, p. 887-890. In Russian.

Astronomy and Astrophysics

Astronomy

Energy Dissipation, Magnetic Flux, Solar Flares, Solar Prominences, Heat Balance, Helioseismology

Scientific paper

It is believed that prominences exist at potential-energy minima (i.e., in 'magnetic holes'). This paper describes observations demonstrating the role played by a preflare prominence (filament) in the occurrence of flares, analyzing a case of an evolving prominence in an active region at the time of the emergence of opposite-polarity magnetic flux. The counterpolar magnetic flux dissipates and heats up the filament and the area underneath; at some moment, the character of the energy loss is changed, disrupting the equilibrium and causing the appearance of a flare.

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