ISOLATING THE FOOTPOINT CHARACTERISTICS OF A SOLAR FLARE LOOP |
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| Authors: | HARRA-MURNION L K CULHANE J L HUDSON H S FUJIWARA T KATO T STERLING A C |
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| Institution: | (1) Mullard Space Science Laboratory, Holmbury St. Mary, Surrey, RH5 6NT, U.K;(2) Institute of Astronomy, University of Hawaii, Honolulu, HI, 96822, U.S.A;(3) Department of Education, Aichi University of Education, Igaya cho, Kariya, 448, Japan;(4) National Institute of Fusion Plasma Science, Nagoya, Japan;(5) Computational Physics Inc., Fairfax, VA, 22031, U.S.A |
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| Abstract: | We analyse the physical characteristics of a C5.7 class flare which was observed on 27 September, 1993 using data from the soft X-ray telescope (SXT), the Bragg crystal spectrometer (BCS), and the hard X-ray telescope (HXT) on Yohkoh. The flare takes the form of a simple loop which is much brighter at one of its footpoints than anywhere else for a period of 2 min. During this time there is an increase in the soft X-ray fluxes, and a corresponding peak in hard X-rays. The parameters derived from the hard X-ray and soft X-ray spectra and images are assumed to be from the footpoint. This flare showed two peaks in the non-thermal velocity, the first one simultaneous with the footpoint brightening. The non-thermal velocity corresponding to these first few minutes is unusually large – by a factor of 80%, 68%, and 26% relative to the second peak in the Fexxv, Caxix, and Sxv channels respectively. |
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