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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/1808
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dc.contributor.authorChoudhuri, A. R-
dc.date.accessioned2007-09-19T09:52:47Z-
dc.date.available2007-09-19T09:52:47Z-
dc.date.issued1996-
dc.identifier.citationBASI, Vol.24 No. 2 pp. 219-222en
dc.identifier.urihttp://hdl.handle.net/2248/1808-
dc.description.abstractThe 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.extent355516 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherAstronomical Society of Indiaen
dc.relation.urihttp://adsabs.harvard.edu/abs/1996BASI...24..219Cen
dc.subjectThe Sunen
dc.subjectMagnetic fields - MHDen
dc.titleMagnetic fields in the sun's interior: What do we know about them?en
dc.typeArticleen
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