Rotational mixing in low-mass stars

Free access article

Issue		A&A Volume 453, Number 1, July I 2006


Page(s)		261 - 278
Section		Stellar structure and evolution
DOI		http://dx.doi.org/10.1051/0004-6361:20053065

A&A 453, 261-278 (2006)
DOI: 10.1051/0004-6361:20053065

II. Self-consistent models of Pop II RGB stars

A. Palacios¹, C. Charbonnel^{2, 3}, S. Talon⁴ and L. Siess¹

¹ Institut d'Astronomie et d'Astrophysique, Université Libre de Bruxelles Campus de la Plaine, Boulevard du Triomphe, CP 226, 1050 Bruxelles, Belgium
e-mail: apalacio@ulb.ac.be; ana.palacios@cea.fr
² Observatoire de Genève, 51 chemin des Maillettes, 1290 Sauverny, Switzerland
³ Laboratoire d'Astrophysique de Toulouse-Tarbes, Observatoire Midi-Pyrénées, 14 Av. E. Belin, 31400 Toulouse, France
⁴ Département de Physique, Université de Montréal, Montréal PQ H3C 3J7, Canada

(Received 15 March 2005 / Accepted 21 February 2006)

Abstract
Aims.In this paper we study the effects of rotation in low-mass, low-metallicity RGB stars.
Methods.We present the first evolutionary models taking into account self-consistently the latest prescriptions for the transport of angular momentum by meridional circulation and shear turbulence in stellar interiors as well as the associated mixing processes for chemicals computed from the ZAMS to the upper RGB. We discuss the uncertainties associated with the physical description of the rotational mixing in detail and carefully study their effects on the rotation profile, diffusion coefficients, structural evolution, lifetimes, and chemical signatures at the stellar surface. We focus in particular on the various assumptions concerning the rotation law in the convective envelope, the initial rotation velocity distribution, the presence of $\mu$ -gradients, and the treatment of the horizontal and vertical turbulence.
Results.This exploration leads to two main conclusions. (1) After completion of the first dredge-up, the degree of differential rotation (and hence mixing) is maximised in the case of a differentially rotating convective envelope (i.e., $j_{{\rm CE}}(r) = {\rm const.}$ ), as anticipated in previous studies. (2) Even with this assumption, and contrary to some previous claims, the present treatment for the evolution of the rotation profile and associated meridional circulation and shear turbulence does not lead to enough mixing of chemicals to explain the abundance anomalies in low-metallicity field and globular cluster RGB stars observed around the bump luminosity.
Conclusions.This study raises questions that need to be addressed in the near future. These include, for example, the interaction between rotation and convection and the trigger of additional hydrodynamical instabilities.

Key words: stars: evolution -- stars: interiors -- stars: rotation -- stars: abundances -- hydrodynamics -- turbulence

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