Convection and the Phenomenon of Kilogauss Magnetic Fields on the Sun

Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/390

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DC Field	Value	Language
dc.contributor.author	Venkatakrishnan, P	-
dc.date.accessioned	2005-04-08T04:19:55Z	-
dc.date.available	2005-04-08T04:19:55Z	-
dc.date.issued	1984	-
dc.identifier.citation	Kodaikanal Observatory Bulletins Series A, Vol. 4, pp. 19-24	en
dc.identifier.issn	0374-3632	-
dc.identifier.uri	http://hdl.handle.net/2248/390	-
dc.description.abstract	The role played by convection in the formation of slender magnetic flux tubes and in the dynamics of the gas within the tube is discussed in the case of simplified models. Convection instability cannot drive systematic downflows whereas convective buffetting of the tube can. The inclusion of heat transport reduces the efficiency of convective collapse for the formation of strong fields. The implications of these two results for the solar magnetic flux is pointed out	en
dc.format.extent	260600 bytes	-
dc.format.mimetype	application/pdf	-
dc.language.iso	en	-
dc.publisher	Indian Institute of Astrophysics, Bangalore	en
dc.subject	Convection	en
dc.subject	Magnetic flux tubes	en
dc.title	Convection and the Phenomenon of Kilogauss Magnetic Fields on the Sun	en
dc.type	Article	en
Appears in Collections:	IIAP Publications Kodaikanal Observatory Bulletins (1905 - 1997 )

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