Evolution of latitude zonal structure of the large-scale magnetic field in solar cycles

Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/3647

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DC Field	Value	Language
dc.contributor.author	Makarov, V. I	-
dc.contributor.author	Sivaraman, K. R	-
dc.date.accessioned	2008-09-16T14:13:19Z	-
dc.date.available	2008-09-16T14:13:19Z	-
dc.date.issued	1989-03	-
dc.identifier.issn	0038-0938	-
dc.identifier.uri	http://hdl.handle.net/2248/3647	-
dc.description.abstract	The latitude zonal component of the large-scale solar magnetic field is analyzed using H-alpha charts for the 1905-1982 period, and the poleward migration of prominences is used to calculate the time of reversal of the polar magnetic field for the 1970-1982 period. It is found that in each hemisphere, the polar, middle latitude, and equatorial zones of the predominant polarity of the large-scale magnetic field can be detected by determining the average latitude of prominence samples referred to one boundary of the large-scale magnetic field. Such prominence samples do not have any regular equatorward drift, and they manifest a poleward migration with a variable velocity of up to 30 m/s, depending on the phase of the cycle.	en
dc.language.iso	en	en
dc.publisher	Springer	en
dc.relation.uri	http://www.springerlink.com/content/ml525g7134354812/	en
dc.subject	Solar cycles	en
dc.subject	Solar magnetic field	en
dc.subject	H alpha line	en
dc.subject	Lines of force	en
dc.subject	Migration	en
dc.subject	Polarity	en
dc.subject	Solar prominences	en
dc.title	Evolution of latitude zonal structure of the large-scale magnetic field in solar cycles	en
dc.type	Article	en
Appears in Collections:	IIAP Publications

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