Inferring the accelerated electron spectrum in solar flares

Details Inferring the accelerated electron spectrum in solar flares Inferring the accelerated electron spectrum in solar flares

Jun 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aipc..374..320l&link_type=abstract

High energy solar physics. AIP Conference Proceedings, Volume 374, pp. 320-328 (1996).

Physics

Solar Electromagnetic Emission

Scientific paper

We invert high spectral resolution hard X-ray observations of the 1980 June 27 solar flare to obtain the parent X-ray-producing electron population. Assuming that collisions are the dominant loss mechanism, the accelerated electron population is derived as a function of time through the flare, using a continuity equation. We find that there appear to be two separate components in the accelerated electrons: an impulsive component with a spectrum peaked at 50 keV, and a slowly varying component with a power-law spectrum extending down to 20 keV.

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