Relations between the toroidal magnetic field in the solar convection zone and the bipolar magnetic field of sunspots
In the solar convection zone, the ..omega..-effect can produce a fairly strong toroidal magnetic field and its magnetic buoyance can result in the ascending motion of certain magnetic field elements. Consequently this process can produce the bipolar magnetic field of sunspots at the surface of the sun. The present paper considers that, owing to the existence of a vertical gradient of the turbulent magnetic diffusion rate in the convection zone, the difference between the magnetic diffusion rate inside and outside the ''bubble'', the magnetic fluid element, is progressively enhanced with height as the bubble moves upward. As a result, at the boundary of the bubble, a large gradient of the magnetic diffusion rate can occur. From the governing equation of magnetic induction, it can be seen that this gradient should perturb the toroidal magnetic field. Consequently, a magnetic ring is formed at the boundary of the bubble. When this ring reaches the top of the convection zone, the magnetic field emerges with two opposite polarities at the surface of the sun. The present paper attempts to use this model to explain the locally concentrated bipolar magnetic field of the sunspots.
- Research Organization:
- Department of Geophysics, Peking University
- OSTI ID:
- 5332713
- Journal Information:
- Chin. Phys.; (United States), Vol. 2:3
- Country of Publication:
- United States
- Language:
- English
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