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

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.