Magnetic fields in the sun's interior: What do we know about them?

dc.contributor.author	Choudhuri, A. R
dc.date.accessioned	2007-09-19T09:52:47Z
dc.date.available	2007-09-19T09:52:47Z
dc.date.issued	1996
dc.identifier.citation	BASI, Vol.24 No. 2 pp. 219-222	en
dc.identifier.uri	http://hdl.handle.net/2248/1808
dc.description.abstract	The surface observations of the solar magnetic fields put some constraints on the possible magnetic configurations in the Sun's interior. It is currently believed that the solar magnetic fields are generated by a dynamo process at the interface between the convection zone and the radiative core. Detailed calculations on the buoyant rise of the magnetic flux from the dynamo region suggest that the strong toroidal field there should have a magnitude of about 10 to the power 5 G. we also discuss a probable configuration of the poloidal field in the convection zone which is consistent with the surface observations.	en
dc.format.extent	355516 bytes
dc.format.mimetype	application/pdf
dc.language.iso	en	en
dc.publisher	Astronomical Society of India	en
dc.relation.uri	http://adsabs.harvard.edu/abs/1996BASI...24..219C	en
dc.subject	The Sun	en
dc.subject	Magnetic fields - MHD	en
dc.title	Magnetic fields in the sun's interior: What do we know about them?	en
dc.type	Article	en