Multiwavelength analysis of a well observed flare from SMM

Details Multiwavelength analysis of a well observed flare from SMM Multiwavelength analysis of a well observed flare from SMM

Sep 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985soph...99..167m&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 99, Sept. 1985, p. 167-188. SERC-supported research.

Physics

23

Solar Flares, Solar Maximum Mission, Solar Spectra, Spectrum Analysis, Extreme Ultraviolet Radiation, H Alpha Line, Light Curve, Magnetic Signatures, Solar X-Rays, Ultraviolet Spectrometers, X Ray Imagery

Scientific paper

Observations of an M 1.4 flare which began at 17:00 UT on November 12, 1980, are presented and analyzed. Ground based H-alpha and magnetogram data have been combined with EUV, soft and hard X-ray observations made with instruments on-board the Solar Maximum Mission satellite. The preflare phase was marked by a gradual brightening of the flare site in O v and the disappearance of an H-alpha filament. Filament ejecta were seen in O v moving southward at a speed of about 60 km/s, before the impulsive phase. The flare loop footpoints brightened in H-alpha and the Ca XIX resonance line broadened dramatically 2 min before the impulsive phase. Nonthermal hard X-ray emission was detected from the loop footpoints during the impulsive phase, while during the same period blue-shifts corresponding to upflows of 200-250 km/s were seen in Ca XIX. Evidence was found for energy deposition in both the chromosphere and corona at a number of stages during the flare. Two widely studied mechanisms for the production of the high temperature soft X-ray flare plasma in the corona are considered, i.e. chromospheric evaporation, and a model in which the heating and transfer of material occurs between flux tubes during reconnection.

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