Convection and the Phenomenon of Kilogauss Magnetic Fields on the Sun

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