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Multiwavelength analysis of a well observed flare from SMMObservations 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.
Document ID
Document Type
Reprint (Version printed in journal)
External Source(s)
Macneice, P. (SERC Rutherford Appleton Laboratory, Didcot, United Kingdom)
Pallavicini, R. (Arcetri Osservatorio Astrofisico, Florence, Italy)
Mason, H. E. (Cambridge University United Kingdom)
Simnett, G. M. (Birmingham, University United Kingdom)
Antonucci, E. (Torino, Universita Turin, Italy)
Shine, R. A. (Science Research Council Didcot, United Kingdom)
Dennis, B. R. (NASA Goddard Space Flight Center Greenbelt, MD, United States)
Date Acquired
August 12, 2013
Publication Date
September 1, 1985
Publication Information
Publication: Solar Physics
Volume: 99
ISSN: 0038-0938
Subject Category
Distribution Limits