On the relationship between soft X-rays and H-alpha-emitting structures during a solar flare

Details On the relationship between soft X-rays and H-alpha-emitting structures during a solar flare On the relationship between soft X-rays and H-alpha-emitting structures during a solar flare

May 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...246..321z&link_type=abstract

Astrophysical Journal, Part 1, vol. 246, May 15, 1981, p. 321-330.

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12

Coronal Loops, H Alpha Line, Solar Corona, Solar Flares, Solar Spectra, Solar X-Rays, Bursts, Energy Dissipation, Skylab Program, Solar Magnetic Field, Solar Prominences, Spectroheliographs, Sunspots, Time Measurement

Scientific paper

Based on data obtained during a solar flare on March 31, 1979, soft X-ray (SXR) and hard X-ray (HXR) bursts are analyzed and compared with other available data in order to identify structures in H-alpha that may correspond to the SXR-emitting site. Measurements taken with the X-ray telescope and the XUV spectroheliograph flown on Skylab, have shown that the SXR emission from many flares comes from rather small structures of about 10-20 arcsec across. These structures appear to be loops that cross the magnetic neutral line. Understanding of the morphology of SXR was based on data of the solar flare of June 15, 1973, observed from Skylab, and the work of Moore et al., (1980). Dense, highly emissive coronal structures, not suggested to be the X-ray source, were forming, lost energy rapidly by emission and conduction, and finally formed the loops. It is concluded that bright H-alpha loops form rapidly as the SXR emission rises, and the overall decay (cooling rate) of SXR emission is much slower than the formation time of individual loops.

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