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Conditions of acceleration of solar electrons, and determination of the magnetic field in the high corona from the characteristics of a type-IV burst

Published online by Cambridge University Press:  14 August 2015

A. Boischot  and
B. Clavelier
A. Boischot
Affiliation:
Observatoire de Paris-Meudon, France
B. Clavelier
Affiliation:
Observatoire de Paris-Meudon, France

Abstract

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The study of a moving type-IV burst shows that acceleration of electrons can happen in the high corona, and a mechanism is proposed for such an acceleration. The low-frequency cut-off of radio spectrum is interpreted as due to the effect of the coronal plasma upon the synchrotron emission, and this leads to an accurate determination of the intensity of the magnetic field at an altitude of 1 R⊙. Then it is possible to compute the energy and the density of the relativistic electrons.

Type
Part VIII: Radio Structure of an Active Region
Information
Symposium - International Astronomical Union , Volume 35: Structure and Development of Solar Active Regions , 1968 , pp. 565 - 569
Copyright
Copyright © Reidel 1968 

References

Boischot, A., Clavelier, B. (1967) Astrophys. Lett., 1, 7.Google Scholar
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Ginzburg, V.L., Syrovatskii, S.I. (1965) A. Rev. Astr. Astrophys., 3, 297.Google Scholar
Kundu, M.R. (1965) Solar Radio Astronomy, Interscience Publishers, New York, p. 383.Google Scholar