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Instabilities and mixing in stellar radiation zones

Published online by Cambridge University Press:  01 April 2008

Jean-Paul Zahn
Jean-Paul Zahn*
Affiliation:
LUTH, Observatoire de Paris, 92195 Meudon, France email: Jean-Paul.Zahn@obspm.fr
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Abstract

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The standard model of stellar structure is unable to account for various observational facts, and there is now a large consensus that some ‘extra mixing’ must occur in the radiation zones. The possible causes for such mixing are briefly reviewed. The most efficient among them is probably the shear-turbulence generated by the differential rotation, which itself results from the transport of angular momentum that can be mediated through the large-scale circulation induced by structural adjustments or by the applied torques (stellar wind, accretion, tides). In solar-type stars this angular momentum transport is ensured mainly by internal gravity waves that are excited at the boundary with convection zones. Another cause of mixing manifests itself in the red giant phase, namely the thermohaline instability due to an inversion of the molecular weight gradient. The implementation of these processes in stellar evolution codes is giving rise to a new generation of stellar models, which are in much better agreement with the observational constraints.

Keywords

Instabilitiesturbulencestars: evolutioninteriorsrotation
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. 47 - 59
Copyright
Copyright © International Astronomical Union 2008

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