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Using the orbiting companion to trace WR wind structures in the 29d WC8d + O8-9IV binary CV Ser

Published online by Cambridge University Press:  12 July 2011

Alexandre David-Uraz  and
Anthony F. J. Moffat
Alexandre David-Uraz
Affiliation:
Département de Physique, Université de Montréal, C.P. 6128, Succursale Centre-Ville, Montréal, QC H3C 3J7, Canada emails: alexandre@astro.umontreal.ca, moffat@astro.umontreal.ca
Anthony F. J. Moffat
Affiliation:
Département de Physique, Université de Montréal, C.P. 6128, Succursale Centre-Ville, Montréal, QC H3C 3J7, Canada emails: alexandre@astro.umontreal.ca, moffat@astro.umontreal.ca
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Abstract

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We have used continuous, high-precision, broadband visible photometry from the MOST satellite to trace wind structures in the WR component of CV Ser over more than a full orbit. Most of the small-scale light-curve variations are likely due to extinction by clumps along the line of sight to the O companion as it orbits and shines through varying columns of the WR wind. Parallel optical spectroscopy from the Mont Megantic Observatory is used to refine the orbital and wind-collision parameters, as well as to reveal line emission from clumps.

Keywords

stars: Wolf-Rayetstars: windsoutflows
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. 499 - 500
Copyright
Copyright © International Astronomical Union 2011

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