Hard X-ray imaging of a solar gradual hard X-ray burst on April 1, 1981

Details Hard X-ray imaging of a solar gradual hard X-ray burst on April 1, 1981 Hard X-ray imaging of a solar gradual hard X-ray burst on April 1, 1981

Sep 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984soph...94..359t&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 94, Sept. 1984, p. 359-367.

Astronomy and Astrophysics

Astronomy

12

Coronal Loops, Solar Flares, Solar X-Rays, X Ray Sources, H Alpha Line, Magnetic Field Configurations, Solar Corona, Solar Electrons, Spaceborne Astronomy

Scientific paper

An intense solar X-ray burst occurred on April, 1981. X-ray images of this gradual hard X-ray burst were observed with the hard X-ray telescope aboard the Hinotori satellite for the initial ten minutes of rise and maximum phases of the burst. The hard X-ray images (13-29 keV) look like a large loop without considerable time variation of an elongated main source during the while observation period. The main X-ray source seems to lie along coronal arcade 20,000 km above a neutral line, while a tongue-like subsource may be another large coronal loop (although the whole structure of the X-ray source looks like a large semicircular loop. Both nonthermal and hot thermal (3-4 x 10 K) electrons are contributing to the source image. The ratio of these components changed in a wide range, from 2.3 to 0.4, during the observation, while the image was rather steady. This suggests that both heating and accelerations of electrons are occurring simultaneously in a common source. Energetic electrons of 15-30 keV would be collisionally trapped in the coronal magnetic loops with density of the order of 10 to the 11th/cu cm.

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