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On Proton and Electron Acceleration by Shock Waves during Large Solar Flares

Published online by Cambridge University Press:  25 April 2016

V. M. Gubchenko  and
V. V. Zaitsev
V. M. Gubchenko
Affiliation:
Applied Physics Institute, Gorky, USSR
V. V. Zaitsev
Affiliation:
Applied Physics Institute, Gorky, USSR
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Extract

Lin and Hudson (1976) have recently analysed non-thermal processes in proton flares, using observations of a series of major events in August 1972. They concluded that the 10–100 keV electrons accelerated during the flash phase account for the bulk of the total energy of a large proton flare (about 1032 – 1033 ergs); that most protons are accelerated later than the 10 — 100 keV electrons; and that most energetic protons escape to the interplanetary medium. Their conclusions with regard to proton acceleration are supported firstly by the delay of the maximum of γ-ray emission by 3-5 minutes after the maximum of X-ray emission, and secondly by the satisfactory agreement between the 7-ray spectrum and the thin-target model of emission. The energetic protons contain a very small fraction of the total flare energy (of the order of 10-5).

Type
Contributions
Information
Publications of the Astronomical Society of Australia , Volume 3 , Issue 3 , 1978 , pp. 236 - 238
Copyright
Copyright © Astronomical Society of Australia 1978

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References

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