Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997azh....74..448t&link_type=abstract
Astronomicheskij Zhurnal, vol. 74, p. 448
Astronomy and Astrophysics
Astronomy
2
Solar Magnetic Field, Solar Convection (Astronomy), Magnetic Field Configurations, Magnetohydrodynamic Turbulence, Diffusion Coefficient, Astronomical Models, Magnetoactivity
Scientific paper
A model for the solar cycle in which the poloidal field is regenerated by the entrainment of a magnetic field in closed circulatory flows is investigated. These flows are concentrated in narrow layers near the base of the convection zone and at the surface, and circulate from the equator to the poles at the surface and from the poles to the equator at the convectiom zone base. A loop of a new poloidal magnetic field forms close to the convection zone base, near the poles. The poloidal field at the upper boundary of the flow is opposite to the poloidal field of the current cycle, and is the source of a field for the new 11-year cycle; the sign of the poloidal field at the lower boundary coincides with the direction of the poloidal field for the current cycle, but this field is confined in a narrow layer between the base of the convection zone and the moving matter. With time, the new poloidal field loop is dragged by the moving flow from the poles to the equator, making the generation of a toroidal field possible via differential rotation and the change in sign of the magnetic field in the 11-year cycle. The characteristic time for the upward floating of the magnetic field captured between the convection zone base and the nearby moving flow layer is much greater than eleven years, so that in this region, the fields from several cycles are superposed and partially compensate each other.
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