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Thermohaline mixing in low-mass giants

Published online by Cambridge University Press:  01 April 2008

M. Cantiello  and
N. Langer
M. Cantiello
Affiliation:
Astronomical Institute Utrecht, Princetonplein 5, 3584 CC Utrecht, The Netherlands email: [email protected], [email protected]
N. Langer
Affiliation:
Astronomical Institute Utrecht, Princetonplein 5, 3584 CC Utrecht, The Netherlands email: [email protected], [email protected]
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Abstract

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Thermohaline mixing has recently been proposed to occur in low mass red giants, with large consequences for the chemical yields of low mass stars. We investigate the role of thermohaline mixing during the evolution of stars between 1 M⊙ and 3 M⊙, in comparison to other mixing processes acting in these stars. We confirm that thermohaline mixing has the potential to destroy most of the 3He which is produced earlier on the main sequence during the red giant stage. In our models we find that this process is working only in stars with initial mass M ≲ 1.5 M⊙. Moreover, we report that thermohaline mixing can be present during core helium burning and beyond in stars which still have a 3He reservoir. While rotational and magnetic mixing is negligible compared to the thermohaline mixing in the relevant layers, the interaction of thermohaline motions with differential rotation and magnetic fields may be essential to establish the time scale of thermohaline mixing in red giants.

Keywords

stars: evolutionstars: abundancesstars: AGB and post-AGBstars: magnetic fieldsstars: rotationISM: abundances
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. 103 - 109
Copyright
Copyright © International Astronomical Union 2008

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