The structure and evolution of a solar flare as observed in 3.5-30 keV X-rays

Details The structure and evolution of a solar flare as observed in 3.5-30 keV X-rays The structure and evolution of a solar flare as observed in 3.5-30 keV X-rays

Apr 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983soph...84..237h&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 84, April 1983, p. 237-261.

Astronomy and Astrophysics

Astronomy

14

Astronomical Photography, Solar Flares, Solar X-Rays, X Ray Astronomy, Astronomical Maps, H Alpha Line, Solar Instruments, Solar Maximum Mission, Time Response

Scientific paper

The complex flare event observed on July 5, 1980, by the Hare X-Ray Imaging Spectrometer on board the Solar Maximum Mission which started at 22:32 UT from AR 2559 (Hale 16955), then at N 28 W 29, and finally developed into a 2-ribbon flare is discussed. The X-ray images are compared with H-alpha photographs taken at the Big Bear Solar Observatory, and the site of the most energetic flare phenomena is determined. It is noted that during the early phases of the event the hard X-rays (exceeding 16 keV) issued from a compact source located near one of the two bright H-alpha kernels. The latter are believed to be the footpoints of a compact magnetic loop. The kernel identified with the X-ray source is immediately adjacent to one of the principal sunspots and in fact is seen as 'rotating' around the sunspot over 90 deg in the early phase of the flare. Two intense X-ray bursts occur at the site of the rotating kernel, and after each burst the loop fills with hot, X-ray-emitting plasma. If the first burst is interpreted as bremsstrahlung from a beam of electrons impinging on a medium that is collisionally dominated, the energy in these electrons is approximately 5 x 10 to the 30th erg.

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