Astronomy and Astrophysics – Astronomy
Scientific paper
Apr 1984
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984azh....61..354k&link_type=abstract
(Astronomicheskii Zhurnal, vol. 61, Mar.-Apr. 1984, p. 354-365) Soviet Astronomy (ISSN 0038-5301), vol. 28, Mar.-Apr. 1984, p. 2
Astronomy and Astrophysics
Astronomy
10
Diamagnetism, Photosphere, Solar Atmosphere, Solar Magnetic Field, Solar Wind, Space Plasmas, Dynamo Theory, Turbulence Effects
Scientific paper
The turbulent viscosity and the large-scale magnetic-field-transfer rate due to turbulent diamagnetism in the solar photosphere and convective zone (CZ) are determined for the Harvard-Smithsonian standard atmosphere (Gingerich et al., 1971) and the convective-zone model of Baker and Temesvary (1966), taking magnetic buoyancy into account. The results are presented in diagrams and graphs and characterized in detail. In the lower CZ, the field is found to descend at rates up to 10 m/s, and the upper limit of the equilibrium field at the CZ base ranges from 2.1 to 700 kG, depending on the float-up mechanism adopted. Fields larger than equilibrium move outward into the subphotosphere, and fields smaller than equilibrium descend to the CZ base; transfer times are shorter than a solar half-cycle. The field-generation rates needed to reproduce the solar cycle are calculated and range from 100 nG/sec to 1 mG/sec, again depending on the buoyancy mechanism used.
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