Evolution of the coronal and transition-zone plasma in a compact flare - The event of 1973 August 9

Details Evolution of the coronal and transition-zone plasma in a compact flare - The event of 1973 August 9 Evolution of the coronal and transition-zone plasma in a compact flare - The event of 1973 August 9

Sep 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...224.1017u&link_type=abstract

Astrophysical Journal, Part 1, vol. 224, Sept. 15, 1978, p. 1017-1027.

Astronomy and Astrophysics

Astrophysics

30

Far Ultraviolet Radiation, Solar Corona, Solar Flares, Solar Wind, Solar X-Rays, Cooling, Skylab Program, Solar Flux Density, Solar Spectra, Solar Temperature

Scientific paper

X-ray and extreme ultraviolet observations of a compact flare were analyzed to determine the relative importance of radiation, thermal conduction, and 'evaporation' in the evolution of the temperature and density structure of the plasma. In the event studied (1973 August 9), the electron density was relatively high (5 x 10 to the eleventh to 1 x 10 to the twelfth) and radiation was evidently an important energy-loss and cooling mechanism. The light curves of ultraviolet lines formed at temperatures between 10 to the fifth to 10 to the seventh K indicate a time-varying emission measure gradient, and hence temperature gradient, during the flare. Radiative instability evidently played an important role in determining the steepness of these gradients during the rise and fall phases, and caused strong downward motions of material during the cooling phase. Toward the end of the event, the coronal electron density decreased and the temperature gradient relaxed toward that expected from a conduction-dominated plasma. For this flare, evaporative cooling did not appear to be a significant factor.

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