Abstract
The evolution of hot thermal plasma in solar flares is analyzed by a single-temperature model applied to continuum emission in the 5 keV < E < 13 keV spectral range. The general trend that the thermal plasma observed in soft X-rays is heated by the non-thermal electrons that emit as the hard X-ray bursts is confirmed by the observation of an electron temperature increase at the time interval of hard X-ray spikes and a quantitative comparison between thermal energy content and hard X-ray energy input. Non-thermal electrons of 10 keV < E < 30 keV energy may play an important role in pre- and post-burst phases.
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© 1983 D. Reidel Publishing Company, Dordrecht, Holland
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Watanabe, T., Tanaka, K., Akita, K., Nitta, N. (1983). Thermal Evolution of Flare Plasma. In: Kane, S.R., Uchida, Y., Tanaka, K., Hudson, H.S. (eds) Recent Advances in the Understanding of Solar Flares. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-7228-5_12
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DOI: https://doi.org/10.1007/978-94-009-7228-5_12
Publisher Name: Springer, Dordrecht
Print ISBN: 978-94-009-7230-8
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