Time variation of the hard X-ray image during the early phase of solar impulsive bursts

Details Time variation of the hard X-ray image during the early phase of solar impulsive bursts Time variation of the hard X-ray image during the early phase of solar impulsive bursts

Oct 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993pasj...45..737t&link_type=abstract

PASJ: Publications of the Astronomical Society of Japan (ISSN 0004-6264), vol. 45, no. 5, p. 737-753

Astronomy and Astrophysics

Astronomy

29

Solar Flares, Solar X-Rays, Variations, X Ray Imagery, X Ray Spectra, Contours, Electron Energy, Magnetic Signatures, Solar Limb, X Ray Detectors

Scientific paper

The time variations of hard X-ray images of four impulsive bursts with simple source structures were investigated in a comparison with the magnetic structure. Two of them are limb bursts. Common variations during the early phase are as follows: (1) The hard X-ray brightening seems to start at the top of a single coronal loop. (2) The X-ray source spreads during the increasing phase of the burst in both directions along the loop, and both ends become brighter, especially at higher energies with generally unequal brightness. The loop top is still bright, especially at lower energies, to show three peaks. The speed of the expansion of the X-ray source amounts to about 104 km/s in three cases. (3) At and after the peak of the X-ray flux, the source tends to be a single source at the loop top, especially at lower energies. (4) The effective temperature for quasi-thermal electrons and their number density during the early phase in the vicinity of the loop top are (4-6) x 107 K and (5-2) x 109/cub cm, respectively, so that the electron mean free path is greater than three-times the local temperature scale height. These observations are consistent with the idea that anomalous resistivity, which triggers impulsive bursts, is caused by electron plasma waves generated in the process of heat conduction.

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