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Cyclic variations in distribution of the coronal green line brightness and solar magnetic field

Published online by Cambridge University Press:  14 March 2005

Olga G. Badalyan ,
V. N. Obridko  and
J. Sýkora
Olga G. Badalyan
Affiliation:
Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation, 142190, Troitsk, Moskow region, Russia email: [email protected]
V. N. Obridko
Affiliation:
Institute of Terrestrial Magnetism, Ionosphere and Radio Wave Propagation, 142190, Troitsk, Moskow region, Russia email: [email protected]
J. Sýkora
Affiliation:
Astronomical Institute of the Slovak Academy of Sciencies, 59060, Tatranska Lomnica, Slovak Rebublic email: [email protected]
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Abstract

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Cyclic variations of the coronal green line brightness (CGLB) are investigated analysing a series of synoptic charts and a special movie assembled of them, covering 1943-2001. Regular changes of the large-scale CGLB distribution in dependence on the phase in the solar cycle are presented. A quantitative relation between the coronal green line intensity $I$ and the total magnetic field strength $B$ is derived for the period 1977-2001; the $B$ was calculated under potential approximation. A simple exponential relation of type $I \propto B^q$ was found to exist between the above two quantities. It is shown that the $q$ exponent may have opposite sign in the equatorial and polar zones. During phases of the solar cycle maxima the $I$ versus $B$ relation is much more complicated and cannot be expressed by such a simple formula.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS223 , June 2004 , pp. 69 - 72
Copyright
© 2004 International Astronomical Union