Steady and fluctuating parts of sun's internal magnetic field

dc.contributor.author	Gokhale, M. H
dc.contributor.author	Hiremath, K. M
dc.date.accessioned	2008-08-19T05:20:52Z
dc.date.available	2008-08-19T05:20:52Z
dc.date.issued	1993-01
dc.identifier.citation	Weiss, 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 – 68	en
dc.identifier.uri	http://hdl.handle.net/2248/3198
dc.description.abstract	We 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.extent	383253 bytes
dc.format.mimetype	application/pdf
dc.language.iso	en	en
dc.publisher	International Astronomical Union	en
dc.relation.ispartofseries	International Astronomical Union Colloquium No. 137
dc.relation.uri	http://adsabs.harvard.edu/abs/1993ASPC...40...66G	en
dc.subject	Magnetic Field Configurations	en
dc.subject	Solar Magnetic Field	en
dc.subject	Solar Activity
dc.subject	Solar Rotation
dc.title	Steady and fluctuating parts of sun's internal magnetic field	en
dc.type	Article	en