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Active Phenomena in the Solar Atmosphere

Published online by Cambridge University Press:  25 April 2016

S.B. Pikel’ner
S.B. Pikel’ner*
Affiliation:
Sternberg Astronomical Institute, Moscow
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Extract

This paper gives a short description and interpretation of some solar magneto-hydrodynamical and plasma phenomena, based mainly on work by the writer and his collaborators (for an extended review see Kaplan et al. 1974).

The magnetic field is considered as the main factor responsible for a number of manifestations of solar activity. At the photospheric level active regions are displayed as plages, i.e., bright areas, seen near the limb. This means that the temperature gradient in plages is smaller than in the undisturbed photosphere. The decrease in gradient is a result of an increase of convective transport of energy.

Type
Invited Papers
Information
Publications of the Astronomical Society of Australia , Volume 2 , Issue 6 , October 1975 , pp. 316 - 317
Copyright
Copyright © Astronomical Society of Australia 1975

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References

Kaplan, S.A., Pikel’ner, S.B., and Tsytovich, V.N. Phys. Reports, 15C, No. 1 (1974).Google Scholar
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