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Hydrodynamical Simulations of Turbulent Convection in a Rotating Red Giant Star

Published online by Cambridge University Press:  01 April 2008

A. Palacios  and
A. S. Brun
A. Palacios
Affiliation:
Université Montpellier II – GRAAL, CNRS – UMR 5024, place Eugène Bataillon, F-34095 Montpellier, France email: palacios@graal.univ-montp2.fr CEA/DSM/IRFU/SAp – L'Orme des Merisiers bât 709 – F-91191 Gif-sur-Yvette (France) email: asbrun@cea.fr
A. S. Brun
Affiliation:
CEA/DSM/IRFU/SAp – L'Orme des Merisiers bât 709 – F-91191 Gif-sur-Yvette (France) email: asbrun@cea.fr
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Abstract

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We present 3-D hydrodynamical simulations of the extended turbulent convective envelope of a low-mass red giant star. These simulations, computed with the ASH code, aim at understanding the redistribution of angular momentum and heat in extended turbulent convection zones of these giant stars. We focus our study on the effects of turbulence and of the rotation rate on the convective patterns and on the distribution of angular momentum within the inner 50% of the convective envelope of such stars.

Keywords

Hydrodynamicsconvectionstars: rotationstars: evolution
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 4 , Symposium S252: The Art of Modeling Stars in the 21st Century , April 2008 , pp. 175 - 182
Copyright
Copyright © International Astronomical Union 2008

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