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Keplerian masses for the most massive stars: the very luminous, hydrogen-rich Wolf-Rayet stars

Published online by Cambridge University Press:  01 August 2006

Anthony F. J. Moffat
Affiliation:
Département de physique, Université de Montréal, C.P. 6128, Succ. C-V, Montréal, QC, H3C 3J7, Canada email: moffat@astro.umontreal.ca, schnurr@astro.umontreal.ca, chene@astro.umontreal.ca, casoli@astro.umontreal.ca, stlouis@astro.umontreal.ca, alfredo@astro.umontreal.ca
Olivier Schnurr
Affiliation:
Département de physique, Université de Montréal, C.P. 6128, Succ. C-V, Montréal, QC, H3C 3J7, Canada email: moffat@astro.umontreal.ca, schnurr@astro.umontreal.ca, chene@astro.umontreal.ca, casoli@astro.umontreal.ca, stlouis@astro.umontreal.ca, alfredo@astro.umontreal.ca
André-Nicolas Chené
Affiliation:
Département de physique, Université de Montréal, C.P. 6128, Succ. C-V, Montréal, QC, H3C 3J7, Canada email: moffat@astro.umontreal.ca, schnurr@astro.umontreal.ca, chene@astro.umontreal.ca, casoli@astro.umontreal.ca, stlouis@astro.umontreal.ca, alfredo@astro.umontreal.ca
Jules Casoli
Affiliation:
Département de physique, Université de Montréal, C.P. 6128, Succ. C-V, Montréal, QC, H3C 3J7, Canada email: moffat@astro.umontreal.ca, schnurr@astro.umontreal.ca, chene@astro.umontreal.ca, casoli@astro.umontreal.ca, stlouis@astro.umontreal.ca, alfredo@astro.umontreal.ca
Nicole St-Louis
Affiliation:
Département de physique, Université de Montréal, C.P. 6128, Succ. C-V, Montréal, QC, H3C 3J7, Canada email: moffat@astro.umontreal.ca, schnurr@astro.umontreal.ca, chene@astro.umontreal.ca, casoli@astro.umontreal.ca, stlouis@astro.umontreal.ca, alfredo@astro.umontreal.ca
Alfredo Villar-Sbaffi
Affiliation:
Département de physique, Université de Montréal, C.P. 6128, Succ. C-V, Montréal, QC, H3C 3J7, Canada email: moffat@astro.umontreal.ca, schnurr@astro.umontreal.ca, chene@astro.umontreal.ca, casoli@astro.umontreal.ca, stlouis@astro.umontreal.ca, alfredo@astro.umontreal.ca
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Abstract

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We propose that the most massive stars in the local Universe start out on the main sequence being extremely luminous and already exhibiting wind-like emission lines. Such stars can probably be identified as hydrogen-rich WN5-7 stars. Masses are now being determined for these stars using the least model-dependent technique of binary orbits.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2007

References

Bonanos, A. Z., Stanek, K. Z., Udalski, A., Wyrzykowski, L., Żebruń, K., Kubiak, M., Szymański, M.K., Szewczyk, O., Pietrzyński, G., & Soszyński, I. 2004, ApJ (Letters), 611, L33CrossRefGoogle Scholar
Rauw, G., De Becker, M., Nazé, Y., Crowther, P. A., Gosset, E., Sana, H., van der Hucht, K. A., Vreux, J.-M., & Williams, P. M. 2004, A&A (Letters), 420, L9Google Scholar
Rauw, G., Crowther, P. A., De Becker, M., Gosset, E., Nazé, Y., Sana, H., van der Hucht, K. A., Vreux, J.-M., & Williams, P. M. 2005, A&A, 432, 985Google Scholar
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Keplerian masses for the most massive stars: the very luminous, hydrogen-rich Wolf-Rayet stars
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