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Boron depletion in 9 to 15 M⊙ stars with rotation

Published online by Cambridge University Press:  23 April 2010

U. Frischknecht ,
R. Hirschi ,
G. Meynet ,
S. Ekström ,
C. Georgy ,
T. Rauscher ,
C. Winteler  and
F.-K. Thielemann
U. Frischknecht
Affiliation:
Department of Physics, University of Basel, CH-4056 Basel, Switzerland email: [email protected]
R. Hirschi
Affiliation:
Astrophysics Group, Keele University, UK-ST5 5BG Keele and Institute for the Physics and Mathematics of the Universe, University of Tokyo, Japan
G. Meynet
Affiliation:
Geneva Observatory, University of Geneva, CH-1290 Sauverny, Switzerland
S. Ekström
Affiliation:
Geneva Observatory, University of Geneva, CH-1290 Sauverny, Switzerland
C. Georgy
Affiliation:
Geneva Observatory, University of Geneva, CH-1290 Sauverny, Switzerland
T. Rauscher
Affiliation:
Department of Physics, University of Basel, CH-4056 Basel, Switzerland email: [email protected]
C. Winteler
Affiliation:
Department of Physics, University of Basel, CH-4056 Basel, Switzerland email: [email protected]
F.-K. Thielemann
Affiliation:
Department of Physics, University of Basel, CH-4056 Basel, Switzerland email: [email protected]
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Abstract

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The treatment of mixing is still one of the major uncertainties in stellar evolution models. One open question is how well the prescriptions for rotational mixing describe the real effects. We tested the mixing prescriptions included in the Geneva stellar evolution code (GENEC) by following the evolution of surface abundances of light isotopes in massive stars, such as boron and nitrogen. We followed 9, 12 and 15 M⊙ models with rotation from the zero age main sequence up to the end of He burning. The calculations show the expected behaviour with faster depletion of boron for faster rotating stars and more massive stars. The mixing at the surface is more efficient than predicted by prescriptions used in other codes and reproduces the majority of observations very well. However two observed stars with strong boron depletion but no nitrogen enrichment still can not be explained and let the question open whether additional mixing processes are acting in these massive stars.

Keywords

Stars: rotationabundancesinteriors
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S268: Light Elements in the Universe , November 2009 , pp. 421 - 422
Copyright
Copyright © International Astronomical Union 2010

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