An interacting loop model for solar flare bursts

Details An interacting loop model for solar flare bursts An interacting loop model for solar flare bursts

Mar 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981ilms.bookr....e&link_type=abstract

Unknown

Physics

Magnetohydrodynamics, Solar Flares, X Ray Sources, Chromosphere, Magnetohydrodynamic Waves, Plasmas (Physics), Solar Spectra

Scientific paper

We show how, as a result of the strong heating produced at chromospheric levels during a solar flare burst, the local gas pressure can transiently attain very large values in certain regions. The effectiveness of the surrounding magnetic field at confining this high pressure plasma is therefore reduced and the flaring loop becomes free to expand laterally. In so doing it may drive magnetic field lines into neighboring, non-flaring, loops in the same active region, causing magnetic reconnection to take place and triggering another flare burst. The features of this interacting loop model are found to be in good agreement with the energetics and time structure of flare-associated solar hard X-ray bursts.

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