EDP Sciences
Free access
Volume 447, Number 1, February III 2006
Page(s) 285 - 292
Section Stellar structure and evolution
DOI http://dx.doi.org/10.1051/0004-6361:20053197
A&A 447, 285-292 (2006)
DOI: 10.1051/0004-6361:20053197

Mixing zones in magnetized differentially rotating stars

V. Urpin1, 2

1  Departament de Fisica Aplicada, Universitat d'Alacant, Ap. Correus 99, 03080 Alacant, Spain
    e-mail: vadim.urpin@uv.es
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

© ESO 2006