Hard X-ray images of possible reconnection in the flare of 21 May, 1980

Details Hard X-ray images of possible reconnection in the flare of 21 May, 1980 Hard X-ray images of possible reconnection in the flare of 21 May, 1980

May 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985soph...97..113s&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 97, May 1985, p. 113-129. Research supported by the Ministry for Education and Science of t

Physics

19

Coronal Loops, H Alpha Line, Solar Flares, Solar Maximum Mission, Solar X-Rays, X Ray Spectroscopy, Electron Density (Concentration), Solar Temperature

Scientific paper

An analysis of the growth of X-ray loops in the flare of May 21, 1980, observed by the hard X-ray spectrometer on board SMM spacecraft, has been carried out with high time resolution in six energy channels from 3.5 to 30 keV. This analysis has revealed that the tops of the loops stay for minutes at a given altitude before, quite abruptly, other loop tops begin to appear above them. One of the jumps in altitude, from about 27,000 to about 45,000 km if the loops extended radially, which occurred quite late in the flare development, is studied in detail. The fact that the tops, of higher loops were first seen in the 22-30 keV energy channel, and only minutes later at lower energies, suggests a new release of energy in a very small volume high in the corona. An initial temperature of at least 50 million K is indicated by the data, inside a volume which may not exceed a few hundred km in diameter. A magnetic reconnenction of previously distended field lines appears to be a likely candidate for the observed phenomenon. Some revised values of the characteristic parameters of the whole system of loops in this flare, which has been the topic of several other studies, are also given.

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