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Where do Be stars stand in the picture of rotational mixing?

Published online by Cambridge University Press:  12 July 2011

Paul R. Dunstall ,
Ines Brott ,
Philip L. Dufton  and
Chris J. Evans
Paul R. Dunstall
Affiliation:
Department of Physics and Astronomy, The Queens University of Belfast, BT7 1NN, Northern Ireland, UK email: [email protected]
Ines Brott
Affiliation:
Astronomical Institute, Utrecht University, Princetonplein 5, NL-3584CC, Utrecht, Netherlands
Philip L. Dufton
Affiliation:
Department of Physics and Astronomy, The Queens University of Belfast, BT7 1NN, Northern Ireland, UK email: [email protected]
Chris J. Evans
Affiliation:
UK Astronomy Technology Centre, Royal Observatory Edinburgh, Blackford Hill, Edinburgh, EH9 3HJ, UK
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Abstract

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Atmospheric parameters and photospheric abundances have been estimated for 60 Be-type stars located in 4 fields over the Magellanic Clouds. Particular attention has been given to the absolute nitrogen abundances to test theories of rotational mixing, an important factor in the evolutionary status of B-type stars, Hunter et al. (2008). The analysis used the non-LTE atmospheric code TLUSTY and required the implementation of a procedure to compensate for possible contamination due to the presence of a circumstellar disc. Through comparison with evolutionary models of fast rotating B-type stars and projected rotational velocity distributions our results support the theory that Be-type stars are typically faster rotators than B stars, but the measured nitrogen enhancements appear to be significantly less than expected for Be stars rotating with velocities greater than 70% of their critical velocity

Keywords

stars: emission-lineBestars: atmospheresstars: rotationstars: evolutionstars: abundances(galaxies:) Magellanic Clouds
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S272: Active OB stars: structure, evolution, mass loss, and critical limits , July 2010 , pp. 85 - 86
Copyright
Copyright © International Astronomical Union 2011

References

Hunter, I., Lennon, D. J., Dufton, P. L., Trundle, C. et al. 2008a, A&A, 479, 541Google Scholar