Volume 425, Number 1, October I 2004
|Page(s)||229 - 242|
|Section||Stellar structure and evolution|
|Published online||10 September 2004|
Transport and mixing in the radiation zones of rotating stars*
I. Hydrodynamical processes
LUTH, Observatoire de Paris, 92195 Meudon, France e-mail: [stephane.mathis;jean-paul.zahn]@obspm.fr
Accepted: 3 June 2004
The purpose of this paper is to improve the modelization of the rotational mixing which occurs in stellar radiation zones, through the combined action of the thermally driven meridional circulation and of the turbulence generated by the shear of differential rotation. The turbulence is assumed to be anisotropic, due to the stratification, with stronger transport in the horizontal directions than in the vertical. The main difference with the former treatments by Zahn ([CITE], A&A, 265, 115) and Maeder & Zahn ([CITE], A&A, 334, 1000) is that we expand here the departures from spherical symmetry to higher order, and include explicitly the differential rotation in latitude, to first order. This allows us to treat simultaneously the bulk of a radiation zone and its tachocline(s). Moreover, we take fully into account the non-stationarity of the problem, which will enable us to tackle the rapid phases of evolution. The system of partial differential equations, which govern the transport of angular momentum, heat and chemical elements, is written in a form which makes it ready to implement in a stellar evolution code. Here the effect of a magnetic field is deliberately ignored; it will be included in forthcoming papers.
Key words: turbulence / stars: evolution / stars: rotation
© ESO, 2004
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