Mar 1987
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987soph..110...11p&link_type=abstract
(Solar Cycle Workshop, 1st, Pasadena, CA, Aug. 17-20, 1986) Solar Physics (ISSN 0038-0938), vol. 110, no. 1, 1987, p. 11-21.
Physics
70
Bipolarity, Dynamo Theory, Magnetic Field Configurations, Solar Magnetic Field, Solar Rotation, Sunspots, Boundary Value Problems, Northern Hemisphere, Turbulent Diffusion
Scientific paper
The recent determination that the angular velocity Ω of the Sun declines downward through the convective zone raises serious questions about the nature of the solar dynamo. The principal qualitative features of the Sun are the azimuthal fields that migrate toward the equator in association with an oscillating poloidal field which reverses at about the time of maximum appearance of bipolar magnetic regions. If Ω decreases downward, or is negligible, the horizontal gradient in Ω produces a dynamo with some of these essential characteristics. There is reason to think that the dynamo is confined to the lower half of the convective zone where α has the opposite sign from the usual (α > 0 in the northern hemisphere) producing equatorward migration but reversing the sign of the associated poloidal field. Meridional circulation may play an essential role in shaping the dynamo. At the present time it is essential to measure Ω accurately and determine the nature of the meridional circulation.
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