Analysis of the magnetic field configuration of a filament-associated flare from X-ray, UV, and optical observations

Details Analysis of the magnetic field configuration of a filament-associated flare from X-ray, UV, and optical observations Analysis of the magnetic field configuration of a filament-associated flare from X-ray, UV, and optical observations

Jul 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984soph...93..337c&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 93, July 1984, p. 337-350. Research supported by the Consiglio Nazionale delle Ricerche.

Physics

8

Coronal Loops, Magnetic Field Configurations, Solar Flares, Solar Magnetic Field, Solar Prominences, Solar X-Rays, H Alpha Line, Magnetic Flux, Solar Maximum Mission, Solar Spectra, Ultraviolet Spectra

Scientific paper

X-ray and ultraviolet observations from SMM of a filament-associated event on November 22, 1980 are examined in conjunction with ground-based optical observations, in order to determine the magnetic field configuration involved in the flaring process. Evidence that the flare was produced by gradual energy release in a large sheared magnetic loop which interacted with another smaller loop is found. Nonthermal processes, as indicated by hard X-ray emission and impulsive UV kernels, were produced in the interaction of the two loops. Although this flare shared some of the characteristics of Long Duration (class II) Events, no indication of a helmet-type configuration, as generally envisaged for class II events, was found. On the contrary, the magnetic configuration of the November 22, 1980 event was more similar to that of a compact (class I) flare, although on a much larger spatial scale and longer time scale.

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