Volume 425, Number 1, October I 2004
|Page(s)||243 - 247|
|Section||Stellar structure and evolution|
|Published online||10 September 2004|
On shear-induced turbulence in rotating stars
LUTH, Observatoire de Paris, 92195 Meudon, France e-mail: [stephane.mathis;jean-paul.zahn]@obspm.fr
2 Institut d'Astronomie et d'Astrophysique, Université Libre de Bruxelles, CP 226, bd. du Triomphe, 1050 Brussels, Belgium e-mail: email@example.com
Accepted: 3 March 2004
We review various prescriptions which have been proposed for the turbulent transport of matter and angular momentum in differentially rotating stellar radiation zones. A new prescription is presented for the horizontal transport associated with the anisotropic shear turbulence which is produced by the differential rotation in latitude; this “β-viscosity” is drawn from torque measurements in the classical Couette-Taylor experiment (Richard & Zahn [CITE], A&A, 347, 734). Its implementation in a stellar evolution code leads to enhanced mixing, as illustrated by models of a rotating main-sequence star of 1.5 solar mass.
Key words: turbulence / stars: evolution
© ESO, 2004
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