Physics
Scientific paper
Nov 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aipc..733..191a&link_type=abstract
MHD COUETTE FLOWS: Experiments and Models. AIP Conference Proceedings, Volume 733, pp. 191-200 (2004).
Physics
Stellar Rotation, Magnetic And Electric Fields, Polarization Of Starlight, Magnetohydrodynamics And Plasmas
Scientific paper
Many main-sequence stars exhibit extensive radiative zones. Some of these may rotate differentially and have large-scale meridional circulations, while the solar radiative core rotates rigidly. We are concerned with three topics: The generation of magnetic fields by a dynamo effect of these large-scale motions, the stability of differential rotation if magnetic fields are present initially, and the formation of the solar tachocline being a thin transition layer from rigid solar-core rotation to differential rotation of the outer convective shell. We conclude that dynamo-generation of magnetic fields is unlikely in stellar radiative envelopes. This finding supports the view that the fields of magnetic Ap stars are fossil. If they do exist from the beginning of the stellar life, they will make a differential rotation unstable if the angular velocity decreases with axis distance. This is the magneto-rotational instability. It is found that the time-scale of turning a differential rotation into a rigid one is about 10-100 million years. In the solar radiative core, the angular velocity gradient is positive and the magneto-rotational instability is not found. Nevertheless, magnetic fields will suppress differential rotation by the Lorentz force and reduce the transition between the differentially rotating outer convection zone and the core to a very thin layer. The field strength of the poloidal core magnetic field has to be of the order of 10 G in order to produce the solar tachocline thickness.
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