Interpreting YOHKOH hard and soft X-ray flare observations

Details Interpreting YOHKOH hard and soft X-ray flare observations Interpreting YOHKOH hard and soft X-ray flare observations

May 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995soph..158..283w&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 158, no. 2, p. 283-299

Physics

47

Coronal Loops, Solar Flares, Solar Physics, Solar X-Rays, Sun, Electron Acceleration, Electrons, Energy Dissipation, Solar Limb, Solar Spectra, X Ray Spectra

Scientific paper

A simple model is presented to account for the Yohkoh flare observations of Feldman et al. (1994), and Masuda (1994). Electrons accelerated by the flare are assumed to encounter the dense, small regions observed by Feldman et al. at the tops of impulsively flaring coronal magnetic loops. The values of electron density and volume inferred by Feldman et al. imply that these regions present an intermediate thick-thin target to the energised electrons. Specifically, they present a thick (thin) target to electrons with energy much less (greater) than Ec where 15 keV less than Ec less than 40 keV. The electrons are either stopped at the loop top or precipitate down the field lines of the loop to the footpoints. Collisional losses of the electrons at the loop top produce the heating observed by Feldman et al. and also some hard X-rays. It is argued that this is the mechanism for the loop-top hard X-ray sources observed in limb flares by Masuda. Adopting a simple model for the energy losses of electrons traversing the dense region and the ambient loop plasma, hard X-ray spectra are derived for the loop-top source, the footpoint sources and the region between the loop top and footpoints. These spectra are compared with the observations of Masuda. The model spectra are found to qualitatively agree with the data, and in particular account for the observed steepening of the loop-top and footpoint spectra between 14 and 53 keV and the relative brightnesses of the loop-top and footpoint sources.

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