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Heating and cooling of the thermal X-ray plasma in solar flares by Ronald L. Moore; Dayton W. Datlowe is a Physics and Astronomy article available to read on EtoBox.

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Characteristic times for heating and cooling of the thermal X-ray plasma in solar flares are estimated from the time profile of the thermal X-ray burst and from the temperature, emission measure and over-all length scale of the flare-heated plasma at thermal X-ray maximum. The heating is assumed to be due to magnetic field reconnection, and the cooling is assumed to be due to heat conduction and radiation. Temperatures and emission measures derived from UCSD OSO-7 X-ray flare observations are used, and length scales are obtained from Big Bear large-scale Ha filtergrams for 17 small (subflare to Class 1) flares. The empirical values obtained for the characteristic times imply (1) that flares are produced by magnetic field reconnection, (2) that conduction cooling of the thermal X-ray plasma dominates radiative cooling and (3) that reconnection heating and conduction cooling of the thermal X-ray plasma are approximately in balance at thermal X-ray maximum. This model in combination with the data gives estimates for the electron number density (101~ cm -3) and the magnetic field strength (10-100 G) in the thermal X-ray plasma and for the total thermal energy generated in a subflare (~

Who reads Heating and cooling of the thermal X-ray plasma in solar flares?

Author

Ronald L. Moore; Dayton W. Datlowe

Publisher

Springer; Springer-Verlag; Kluwer Academic Publishers; Springer Science and Business Media LLC (ISSN 0038-0938)

Published

1975

Language

EN

Field

Physics and Astronomy (Physical Sciences)