The relations between the toroidal magnetic field in the solar convection zone and the bipolar magnetic field of sunspots

Details The relations between the toroidal magnetic field in the solar convection zone and the bipolar magnetic field of sunspots The relations between the toroidal magnetic field in the solar convection zone and the bipolar magnetic field of sunspots

Sep 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982acaps...1..188z&link_type=abstract

(Acta Astrophysica Sinica, vol. 1, July 1981, p. 188-196.) Chinese Physics, vol. 2, July-Sept. 1982, p. 668-676. Translation.

Physics

Convective Flow, Magnetic Field Configurations, Solar Activity Effects, Solar Atmosphere, Solar Magnetic Field, Sunspots, Atmospheric Turbulence, Bubbles, Buoyancy, Magnetic Diffusion, Magnetic Induction, Solar Granulation, Toroids

Scientific paper

It is contended that the buoyant bubble, the magnetic fluid element, forming a sunspot should have a dimension no less than the scale length of the sunspot but comparable to the structure of the supergranulation. From the turbulent characteristics of the decay time of the sunspot magnetic field, it is thought that the buoyant motions of the bubble may be described in terms of the mean flow. Since in the solar convective zone the turbulent magnetic diffusion rate has a perpendicular gradient, the difference between the magnetic diffusion rates inside and outside the bubble increases as it moves upward. This can produce a gradient of the diffusion rate at the surface of the bubble which, according to the equation of magnetic induction, can perturb the toroidal magnetic field and eventually form a magnetic ring at the surface of the bubble. As it reaches the surface of the solar convective zone, a bipolar magnetic region is seen. An attempt is made to explain the intensity of the bipolar magnetic field associated with sunspots based on such a process.

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