The 1991 October 24 flare: A challenge for standard models

Details The 1991 October 24 flare: A challenge for standard models The 1991 October 24 flare: A challenge for standard models

Feb 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...440..386d&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 440, no. 1, p. 386-393

Astronomy and Astrophysics

Astronomy

8

Gamma Ray Astronomy, H Alpha Line, Magnetic Field Reconnection, Solar Flares, Solar Magnetic Field, Spaceborne Astronomy, Stellar Models, X Ray Astronomy, Chromosphere, Coronal Loops, Japanese Spacecraft, Light Curve, Magnetic Signatures, Mathematical Models, Solar X-Rays, X Ray Telescopes

Scientific paper

The M9.8 solar flare of 1991 October 24 22:30 UT presents several interesting characteristics: (1) energy release starts high in the corona; (2) the primary chromospheric ribbons are initially well separated and do not move apart at an observable rate; (3) no evidence is found for an erupting filament or other driver. To explain this flare, we consider several canonical flare models, including a filament eruption, a confined filament eruption, current interruption, and interacting loops. We conclude that none of these scenarios unequivocally explains this flare. Two possibilities which cannot be ruled out are (1) the eruption of a filament unobservable in H-alpha which starts high in the corona and produces no ribbon motions smaller than our detection threshold and no perceptible expansion of the coronal X-ray source, and (2) energy release due to spontaneous, propagating reconnection which allows the system to essentially brighten in place.

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