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The migration of sunspot activity along solar meridians and parallels

Published online by Cambridge University Press:  14 August 2015

L. Dezsö ,
O. Gerlei  and
Ágnes Kovács
L. Dezsö
Affiliation:
Heliophysical Observatory of the Hungarian Academy of Sciences, Debrecen, Hungary
O. Gerlei
Affiliation:
Heliophysical Observatory of the Hungarian Academy of Sciences, Debrecen, Hungary
Ágnes Kovács
Affiliation:
Heliophysical Observatory of the Hungarian Academy of Sciences, Debrecen, Hungary

Abstract

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The places of local maxima of sunspot activity, i.e. the formation of solar active regions, seem to follow in a definite sequence of tracks over the Sun's surface. These sequences of activity apparently represent distinct continuous streams, whose duration may be of the order of magnitude of 1 year.

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. 70 - 76
Copyright
Copyright © Reidel 1968 

References

Bell, B. (1960) ‘On the Structure of the Sunspot Zone’, Smithson. Contr. Astrophys., 5.Google Scholar
Dezsö, L. (1964) ‘Statistical Investigations of Sunspots by a New Method’, Publ. Debrecen Obs., 1.Google Scholar
Kuleshova, K.F. (1962) ‘The Fine Structure of the Spot-Formation Zones’, Astr. Zu., 39, 273–277 (= Soviet Astr. - AJ., 6, 213–216).Google Scholar
Lockyer, W.J.S. (1904) ‘Sunspot Variation in Latitude 1861–1902’, Proc. Roy. Soc., 73, 142–152.Google Scholar