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Journal of Physical Studies 11(4), 427–431 (2007)
DOI: https://doi.org/10.30970/jps.11.427 ON THE MOTION OF THE AZIMUTHAL MAGNETIC FIELD IN THE SOLAR CONVECTIVE ZONE AND REGIONS ADJOINING ITP. G. Brayko
Kirovograd National Technical University |
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Helioseismic studies allow to estimate a magnetic field amplitude. These fields appear by the $Ω$-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 $10^5$ 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.
PACS number(s): 90.60.-j, 90.60.Hv, 90.60.Ly