Atomic diffusion in star models of type earlier than G

Free access article

Issue		A&A Volume 390, Number 2, August I 2002


Page(s)		611 - 620
Section		Formation, structure and evolution of stars
DOI		http://dx.doi.org/10.1051/0004-6361:20020768

A&A 390, 611-620 (2002)
DOI: 10.1051/0004-6361:20020768

Atomic diffusion in star models of type earlier than G

P. Morel and F. Thévenin

Département Cassini, UMR CNRS 6529, Observatoire de la Côte d'Azur, BP 4229, 06304 Nice Cedex 4, France

(Received 7 February 2002 / Accepted 15 May 2002 )

Abstract
We introduce the mixing resulting from the radiative diffusivity associated with the radiative viscosity in the calculation of stellar evolution models. We find that the radiative diffusivity significantly diminishes the efficiency of the gravitational settling in the external layers of stellar models corresponding to types earlier than $\approx$ G. The surface abundances of chemical species predicted by the models are successfully compared with the abundances determined in members of the Hyades open cluster. Our modeling depends on an efficiency parameter, which is evaluated to a value close to unity, that we calibrate in this study.

Key words: diffusion -- stars: abundances -- stars: evolution -- Hertzsprung-Russell (HR) and C-M diagrams

Offprint request: P. Morel, Pierre.Morel@obs-nice.fr

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