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Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/3198
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dc.contributor.authorGokhale, M. H-
dc.contributor.authorHiremath, K. M-
dc.date.accessioned2008-08-19T05:20:52Z-
dc.date.available2008-08-19T05:20:52Z-
dc.date.issued1993-01-
dc.identifier.citationWeiss, Werner W and Baglin, Annie. eds., Inside the stars; Proceedings of the 137th IAU Colloquium, Univ. of Vienna, Austria, Apr. 13 - 18, 1992, pp. 66 – 68en
dc.identifier.urihttp://hdl.handle.net/2248/3198-
dc.description.abstractWe have modeled the 'steady' part of sun's internal poloidal magnetic field in the form of a central dipole and a central hexapole with strengths (0.6 +/- 0.1)B(o)R(0) exp 3 and (0.16 +/- 0.05)B(o)R(0) exp 5 embedded in an asymptotically uniform field B(o). A small deviation from isorotation seems to indicate: (i) a slow buildup of toroidal field near the base of the convection zone and (ii) the presence of torsional MHD perturbations in the outer radiative core, with latitudinal structure and time scales which may be similar to those of solar activity.en
dc.format.extent383253 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoenen
dc.publisherInternational Astronomical Unionen
dc.relation.ispartofseriesInternational Astronomical Union Colloquium No. 137-
dc.relation.urihttp://adsabs.harvard.edu/abs/1993ASPC...40...66Gen
dc.subjectMagnetic Field Configurationsen
dc.subjectSolar Magnetic Fielden
dc.subjectSolar Activity-
dc.subjectSolar Rotation-
dc.titleSteady and fluctuating parts of sun's internal magnetic fielden
dc.typeArticleen
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