Coronal magnetic field structure in two-ribbon solar flare on October 16, 1993.

Details Coronal magnetic field structure in two-ribbon solar flare on October 16, 1993. Coronal magnetic field structure in two-ribbon solar flare on October 16, 1993.

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997kfnt...13f..33y&link_type=abstract

Kinematika Fiz. Nebesn. Tel, Tom 13, No. 6, p. 33 - 43

Physics

Solar Corona: Solar Magnetic Fields, Solar Corona: Solar Flares, Solar Flares: Magnetic Reconnection

Scientific paper

A model of the magnetic field configuration in a two-ribbon flare is presented. The model is based on the reconnection of two large-scale closed magnetic field structures. Unlike of the Kopp and Pneuman configuration, the model does not suggest destabilization and eruption of the active region filament. Calculations of coronal linear force-free field show that the necessary magnetic structure exist in the corona. Chromospheric flare ribbons in the two-ribbon flare are located on the intersection of the separatrices with the chromosphere. This inference strongly supports the idea that some two-ribbon flares are due to reconnection process between two (or more) large-scale closed magnetic field structures.

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