Hostname: page-component-586b7cd67f-t7czq Total loading time: 0 Render date: 2024-11-27T06:35:02.222Z Has data issue: false hasContentIssue false
  • English
  • Français

New observational results on the colliding wind WR+O binary WR 30a

Published online by Cambridge University Press:  25 May 2016

Eric Gosset ,
Pierre Royer ,
Gregor Rauw ,
Jean Manfroid  and
Jean-Marie Vreux
Eric Gosset
Affiliation:
Institut d'Astrophysique et de Géophysique, Université de Liège, avenue de Cointe, 5, B-4000 Liège, Belgium
Pierre Royer
Affiliation:
Institut d'Astrophysique et de Géophysique, Université de Liège, avenue de Cointe, 5, B-4000 Liège, Belgium
Gregor Rauw
Affiliation:
Institut d'Astrophysique et de Géophysique, Université de Liège, avenue de Cointe, 5, B-4000 Liège, Belgium
Jean Manfroid
Affiliation:
Institut d'Astrophysique et de Géophysique, Université de Liège, avenue de Cointe, 5, B-4000 Liège, Belgium
Jean-Marie Vreux
Affiliation:
Institut d'Astrophysique et de Géophysique, Université de Liège, avenue de Cointe, 5, B-4000 Liège, Belgium

Extract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

WR30a (MS 4) was first suspected as a possible Wolf-Rayet star by McConnell & Sanduleak (1970) during a deep objective-prism survey performed around the Carina Nebula region. From subsequent studies, the spectrum turned out to be composite, with a WR component classified W04 (or alternatively WC4, W05 and WC3) and an 0 component classified 04. Niemela (1995) reported the first, and up-to-now unique, radial velocity study for that star. She noticed large variations of CIV λ4658 from night to night, suggesting that WR30a might be a short period binary. A plot of the C IV emission-line velocities versus the He II absorption ones clearly indicates that they are exhibiting opposite binary motions. The apparent velocity amplitudes imply a rather low mass ratio Mwo4/Mo4 = 0.15, although the radial velocities of the C IV line could be distorted due to line-profile variations.

Type
Part 3. Interaction of Wolf-Rayet stars and other hot massive stars with their environment: colliding winds and ring nebulae
Information
Symposium - International Astronomical Union , Volume 193: Wolf-Rayet Phenomena in Massive Stars and Starburst Galaxies , 1999 , pp. 354 - 355
Copyright
Copyright © Astronomical Society of the Pacific 1999 

References

McConnell, D.J., Sanduleak, N. 1970, PASP 82, 80 CrossRefGoogle Scholar
Niemela, V.S. 1995, in: van der Hucht, K.A. & Williams, P.M. (eds.), Wolf-Rayet Stars: Binaries, Colliding Winds, Evolution, Proc IAU Symposium No. 163 (Dordrecht: Kluwer), 223 Google Scholar