The site, size, spatial stability, and energetics of an X-ray flare kernel

Details The site, size, spatial stability, and energetics of an X-ray flare kernel The site, size, spatial stability, and energetics of an X-ray flare kernel

Jan 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...227..299p&link_type=abstract

Astrophysical Journal, Part 1, vol. 227, Jan. 1, 1979, p. 299-306.

Astronomy and Astrophysics

Astronomy

6

Plasma Dynamics, Solar Atmosphere, Solar Flares, Solar X-Rays, Spaceborne Astronomy, Stellar Structure, Loops, Radiant Flux Density, Sites, Size Determination, Skylab Program, X Ray Telescopes

Scientific paper

The site, size evolution, and energetics of an X-ray kernel that dominated a solar flare during its rise and somewhat during its peak are investigated. The position of the kernel remained stationary to within about 3 arc sec over the 30-min interval of observations, despite pulsations in the kernel X-ray brightness in excess of a factor of 10. This suggests a tightly bound, deeply rooted magnetic structure, more plausibly associated with the near chromosphere or low corona rather than with the high corona. The H-alpha flare onset coincided with the appearance of the kernel, again suggesting a close spatial and temporal coupling between the chromospheric H-alpha event and the X-ray kernel. At the first kernel brightness peak its size was no larger than about 2 arc sec, when it accounted for about 40% of the total flare flux. In the second rise phase of the kernel, a source power input of order 2 times 10 to the 24th ergs/sec is minimally required.

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