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Last phases of development of active regions

Published online by Cambridge University Press:  14 August 2015

V. Bumba ,
J. Kleczek ,
J. Olmr ,
B. Růžičková-Topolová  and
J. Sýkora
V. Bumba
Affiliation:
Astronomical Institute, Ondřejov
J. Kleczek
Affiliation:
Astronomical Institute, Ondřejov
J. Olmr
Affiliation:
Astronomical Institute, Ondřejov
B. Růžičková-Topolová
Affiliation:
Astronomical Institute, Ondřejov
J. Sýkora
Affiliation:
Astronomical Institute, Skalnaté Pleso, Czechoslovakia

Abstract

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A close relation of filament feet to the supergranular structure has been found. Green corona brightness, 1420 MHz flux, and the location of quiescent filaments depend upon the distribution of the photospheric magnetic fields. The development of polar maxima of the green corona and their relation to the following polarity have been studied.

Type
Part I: General Development of an Active Region
Information
Symposium - International Astronomical Union , Volume 35: Structure and Development of Solar Active Regions , 1968 , pp. 64 - 67
Copyright
Copyright © Reidel 1968 

References

Kiepenheuer, K.O. (1953) in The Sun, Ed. by Kuiper, G.P., The University of Chicago Press, p. 434.Google Scholar