Model of 'steady' Parts of Rotation and Magnetic Field in the Sun's Convection Zone

dc.contributor.author	Hiremath, K. M
dc.contributor.author	Gokhale, M. H
dc.date.accessioned	2008-11-15T12:03:42Z
dc.date.available	2008-11-15T12:03:42Z
dc.date.issued	1995-06
dc.identifier.citation	ESA Proceedings, Vol. 376, pp. 97 - 98	en
dc.identifier.uri	http://hdl.handle.net/2248/4010
dc.description.abstract	We present a preliminary model of the ‘steady’ parts of rotation and magnetic field in the sun’s convective envelope, which vary on diffusion time scales, within the frame work of axisymmetric incompressible hydromagnetics (Ref. 1). We use the boundary conditions for rotation and magnetic field similar to those used by Nakagawa (Ref. 2). The model yields a quadrupole type part in the distribution of the toroidal field whose strength varies from ~ 1 G below the surface to ~ 10/sup 4 G near the base of the convection zone. The model also yields isorotation contours similar to those given by helioseismology.	en
dc.language.iso	en	en
dc.publisher	European Space Agency	en
dc.relation.uri	http://adsabs.harvard.edu/abs/1995ESASP.376b..97H	en
dc.subject	Sun’s Rotation	en
dc.subject	Sun’s Toroidal Magnetic Field	en
dc.title	Model of 'steady' Parts of Rotation and Magnetic Field in the Sun's Convection Zone	en
dc.type	Article	en