EDP Sciences
Free Access
Volume 470, Number 3, August II 2007
Page(s) 1013 - 1022
Section Stellar structure and evolution
DOI https://doi.org/10.1051/0004-6361:20077263

A&A 470, 1013-1022 (2007)
DOI: 10.1051/0004-6361:20077263

The dynamics of a fully radiative rapidly rotating star enclosed within a spherical box

F. Espinosa Lara and M. Rieutord

Laboratoire d'Astrophysique de Toulouse et Tarbes, UMR 5572, CNRS et Université Paul Sabatier Toulouse 3, 14 avenue E. Belin, 31400 Toulouse, France
    e-mail: rieutord@ast.obs-mip.fr

(Received 9 February 2007 / Accepted 22 April 2007)

Context.Recent results from interferometry and asteroseismology require models of rapidly rotating stars that are more and more precise.
Aims. We describe the basic structure and the hydrodynamics of a fully radiative star as a preliminary step towards more realistic models of rotating stars.
Methods. We consider a solar mass of perfect gas enclosed in a spherical container. The gas is self-gravitating and rotating, and is the seat of nuclear heating, and heat diffusion is due to radiative diffusion with Kramers type opacities. Equations are solved numerically with spectral methods in two dimensions with a radial Gauss-Lobatto grid and spherical harmonics.
Results. We computed the centrifugally flattened structure of such a star: the von Zeipel model, which says that the energy flux is proportional to the local effective gravity is tested. We show that it overestimates the ratio of the polar to the equatorial energy flux by almost a factor 2. We also determine the Brunt-Väisälä frequency distribution and show that outer equatorial regions in a radiative zone are convectively unstable when the rotation is fast enough. We compute the differential rotation and meridional circulation stemming from the baroclinicity of the star and show that, in such radiative zones, equatorial regions rotate faster than polar ones. The surface differential rotation is also shown to reach a universal profile when rotation is slow enough (less than 36% of the breakup one), as long as viscosity and Prandlt number remain small.

Key words: hydrodynamics -- stars: rotation

© ESO 2007

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