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22-years magnetic cycle in polar activity of the Sun

Published online by Cambridge University Press:  14 March 2005

V.I. Makarov
Affiliation:
Pulkovo Astronomical Observatory, St.Petersburg, Russia, email: makarov@gao.spb.ru
A.G. Tlatov
Affiliation:
Kislovodsk Solar Station of the Pulkovo Observatory, Russia, email: solar@narzan.ru
J. Singh
Affiliation:
Indian Institute of Astrophysics, Bangalore, India, email: jsingh@iiap.ernet.in
S.S. Gupta
Affiliation:
Indian Institute of Astrophysics, Bangalore, India, email: jsingh@iiap.ernet.in
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Abstract

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We have digitized and processed the daily K-CaII-line full disk spectroheliograms from the archive of the Kodaikanal Observatory during 1907-1995. The programm has been worked out to determine the boundaries of the bright areas (plages, decayed plages, enhanced network features, K-CaII bright points and so on) with contrast that exceeded a level of the quiet Sun on the given value. About the $1.2\,{\times}\,10^6$ K-CaII active regions of different scales were processed. The coordinates, areas, the tilt and latitude-time distributions of bright features were determined. At the high latitudes the K-CaII bright points form a polar branch of solar activity at the period between the polar magnetic field reversals. This polar activity shows both 11-year's and 22-year's cycles. We found that the polar K-CaII bright point cycles proceed on average 5.5 years the sunspot cycles.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Type
Contributed Papers
Copyright
© 2004 International Astronomical Union