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The masses of late-type WN stars

Published online by Cambridge University Press:  01 August 2006

Götz Gräfener  and
Wolf-Rainer Hamann
Götz Gräfener
Affiliation:
Department of Physics, University of Potsdam, D-14469 Postdam, Germany email: goetz@astro.physik.uni-potsdam.de, wrh@astro.physik.uni-potsdam.de
Wolf-Rainer Hamann
Affiliation:
Department of Physics, University of Potsdam, D-14469 Postdam, Germany email: goetz@astro.physik.uni-potsdam.de, wrh@astro.physik.uni-potsdam.de
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Abstract

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We present recent results for galactic WNL stars, obtained with the new Potsdam Wolf-Rayet (PoWR) hydrodynamic model atmospheres. Based on a combination of stellar wind modeling and spectral analysis we identify the galactic WNL subtypes as a group of extremely luminous stars close to the Eddington limit. Their luminosities imply progenitor masses around 120 M⊙ or even above, making them the direct descendants of the most massive stars in the galaxy. Because of the proximity to the Eddington limit our models are very sensitive to the L/M ratio, thus allowing for a direct estimate of the present masses of these objects.

Keywords

stars: mass lossstars: windsoutflowsstars: Wolf-Rayet
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Highlights of Astronomy 14: Highlights of Astronomy , August 2006 , pp. 199
Copyright
Copyright © International Astronomical Union 2007

References

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