Purely coronal flare-like variations

Details Purely coronal flare-like variations Purely coronal flare-like variations

Jun 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983soph...85..313s&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 85, June 1983, p. 313-337. Research supported by the Koninklijke Nederlandse Akademie van W

Astronomy and Astrophysics

Astronomy

25

Magnetic Field Configurations, Polarized Radiation, Solar Corona, Solar Flares, Solar X-Rays, Brightness Distribution, Fine Structure, Solar Atmosphere, Spaceborne Astronomy

Scientific paper

Quasiperiodic X-ray, UV, microwave, and metric-wave variations after a solar flare on November 6, 1980 are reported and analyzed, based on observational data from SMM (HXRBS, UVSP, HXIS), GOES-2, the 100-m radiotelescope at Bonn, and the Nancay radioheliograph. The maxima of the 13 brightenings observed are listed and characterized; a comparison is made with a 'normal' flare at 17:26 UT on the same day. The HXIS and UVSP data are discussed in terms of the physical properties, X-ray flux, O V flux, and H-alpha flux. The variations are found to be mainly thermal and purely coronal, with no chromospheric (H-alpha) participation (in contrast to the 17:26 flare). Since strong X-ray emissions were observed which should have involved the chromosphere through magnetic-field-line heat conduction, it is proposed that the variations wre produced ina coronal plasmoid magnetically separate from the chromosphere. A mechanism for the evolution of such a plasmoid from the upper loops of a giant X-ray arch is discussed. An iterative HXIS-image-deconvolution process is presented in an appendix.

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