Mixing zones in magnetized differentially rotating starsV. Urpin1, 2
1 Departament de Fisica Aplicada, Universitat d'Alacant, Ap. Correus 99, 03080 Alacant, Spain
2 A. F. Ioffe Institute of Physics and Technology and the Isaac Newton Institute of Chili, Branch in St. Petersburg, 194021 St. Petersburg, Russia
(Received 5 April 2005 / Accepted 28 September 2005)
We study the secular instability of magnetized differentially rotating radiative zones taking account of viscosity and magnetic and thermal diffusivities. This considered instability generalizes the well-known Goldreich-Schubert-Fricke instability for the case of a sufficiently strong magnetic field. In magnetized stars, instability can lead to formation of non-spherical, unstable zones where weak turbulence mixes the material between the surface and interiors. Such unstable zones can manifest themselves by a non-spherical distribution of elements on the stellar surface.
Key words: magnetohydrodynamics (MHD) -- instabilities -- magnetic fields -- turbulence
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