Solar hard X-ray emission resulting from an initially homogeneous and isotropic coronal electron population

Details Solar hard X-ray emission resulting from an initially homogeneous and isotropic coronal electron population Solar hard X-ray emission resulting from an initially homogeneous and isotropic coronal electron population

May 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...245..262m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 245, no. 1, May 1991, p. 262-270.

Astronomy and Astrophysics

Astrophysics

3

Solar Corona, Solar Flares, Solar X-Rays, X Ray Spectra, Coronal Loops, Electron Energy, Magnetic Field Configurations, Normal Density Functions, Solar Magnetic Field

Scientific paper

It is proposed that solar flare hard X-rays are produced by a dilute population of electrons which are accelerated simultaneously throughout the coronal part of a flaring loop. The electrons are assumed to have an initially Maxwellian distribution, and the coronal magnetic field is taken to be uniform. Collisions and wave-particle interactions in the corona are neglected. Simple analytical expressions are obtained for the flux of fast electrons escaping from the ends of the loop (i.e., precipitating into the chromosphere), the electric current resulting from this precipitation process, the thick-target hard X-ray emission produced by precipitating electrons, and the hard X-ray emission produced by electrons remaining in the corona. It is pointed out that the current produced by escaping electrons can be neutralized by a partial leakage of electrons from the chromosphere. The model predicts a spectral softening and a reduction in the ratio of coronal to thick-target hard X-rays during the decay phase of impulsive hard X-ray spikes. It is shown that subsecond variations in hard X-ray emission can be reconciled with observations which indicate that a significant fraction of the radiation is coronal in origin.

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