ON THE MOTION OF THE AZIMUTHAL MAGNETIC FIELD IN THE SOLAR CONVECTIVE ZONE AND REGIONS ADJOINING IT

Helioseismic studies allow to estimate a magnetic field amplitude. These fields appear by the a-effect stretch on the initial ones. So, there is a possibility to transport the strong magnetic fields by meridional circulation to the equator without the use of dynamo-waves. It is necessary either to attract the initial fields by a size of 10-100 G, or look over the generation mechanism for the formation of the toroidal magnetic fields with the magnitude 105 G. A radial motion of the powerful magnetic fields is caused by the nonlinear effects of buoyancy and turbulent diamagnetism that are to set a balance on the verge of the radiative and convective. Conditions are found, at which higher equipartition fields can lie under the convective zone and emergte to the surface.