Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984azh....61..540k&link_type=abstract
(Astronomicheskii Zhurnal, vol. 61, May-June 1984, p. 540-548) Soviet Astronomy (ISSN 0038-5301), vol. 28, May-June 1984, p. 316
Astronomy and Astrophysics
Astronomy
7
Atmospheric Turbulence, Dynamo Theory, Solar Atmosphere, Solar Magnetic Field, Angular Velocity, Magnetic Field Configurations, Reynolds Number, Velocity Distribution
Scientific paper
Mixing-length approximations are applied to construct a theoretical model of magnetic-field generation in the turbulent solar envelope. The angular velocity (omega) and helicity (alpha) are calculated as functions of the solar radius, and it is found that omega increases with increasing convective-zone depth, while the alpha effect changes sign in the lower convective zone (from positive to negative in the Northern Hemisphere) when the nonuniform character of the turbulent pulsations are taken into account. It is concluded that the conditions for efficient generation of large-scale magnetic fields by the alpha-omega dynamo mechanism are best met in a layer of varying extent at the center of the convective zone, with maximum intensity for the poloidal and toroidal fields in the upper and lower halves of the zone, respectively, and propagation through the rest of the zone by turbulent diffusion.
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