We present the first visual orbit for the nitrogen-rich Wolf-Rayet binary, WR 133 (WN5o + O9I), based on observations made with the CHARA Array and the MIRC-X combiner. This orbit represents the first visual orbit for a WN star and only the third Wolf-Rayet star with a visual orbit. The orbit has a period of 112.8 days, a moderate eccentricity of 0.36, and a separation of a = 0.79 mas on the sky. We combine the visual orbit with an SB2 orbit and Gaia parallax to find that the derived masses of the component stars are MWR = 9.3 ±1.6M⊙ and MO = 22.6 ±3.2M⊙, with the large errors owing to the nearly face-on geometry of the system combined with errors in the spectroscopic parameters. We also derive an orbital parallax that is identical to the G...
We present the results of an optical spectroscopic study of the massive Wolf-Rayet binary WR137. The...
Context. A significant number of the Wolf-Rayet stars seem to be binary or multiple systems, but the...
Computational models of Wolf-Rayet and other massive stars are presented at solar metallicity and at...
International audienceWe present the first visual orbit for the nitrogen-rich Wolf-Rayet binary, WR ...
We present updated orbital elements for the Wolf-Rayet (WR) binary WR 140 (HD 193793; WC7pd + O5.5fc...
Double-lined spectroscopic binary systems, containing a Wolf-Rayet and a massive O-type star, are ke...
Context. Massive Wolf-Rayet (WR) stars are evolved massive stars (Mi ≳ 20 M⊙) characterized by stron...
Wolf-Rayet (WR) stars represent one of the final stages of massive stellar evolution. Relatively lit...
The results of an extensive spectroscopic campaign on the eclipsing binary WR22 are presented. A new...
Context. BAT99 126 is a multiple system in the Large Magellanic Cloud containing a Wolf-Rayet (WR) s...
Context. Most massive stars reside in multiple systems that will interact over the course of their l...
Wolf–Rayet (WR) stars represent one of the final stages of massive stellar evolution. Relatively lit...
Context. Massive-binary evolution models predict that some systems will go through an evol...
© ESO, 2017. We present the first SB2 orbital solution and disentanglement of the massive Wolf-Raye...
Context. Most massive stars reside in multiple systems that will interact over the course of their l...
We present the results of an optical spectroscopic study of the massive Wolf-Rayet binary WR137. The...
Context. A significant number of the Wolf-Rayet stars seem to be binary or multiple systems, but the...
Computational models of Wolf-Rayet and other massive stars are presented at solar metallicity and at...
International audienceWe present the first visual orbit for the nitrogen-rich Wolf-Rayet binary, WR ...
We present updated orbital elements for the Wolf-Rayet (WR) binary WR 140 (HD 193793; WC7pd + O5.5fc...
Double-lined spectroscopic binary systems, containing a Wolf-Rayet and a massive O-type star, are ke...
Context. Massive Wolf-Rayet (WR) stars are evolved massive stars (Mi ≳ 20 M⊙) characterized by stron...
Wolf-Rayet (WR) stars represent one of the final stages of massive stellar evolution. Relatively lit...
The results of an extensive spectroscopic campaign on the eclipsing binary WR22 are presented. A new...
Context. BAT99 126 is a multiple system in the Large Magellanic Cloud containing a Wolf-Rayet (WR) s...
Context. Most massive stars reside in multiple systems that will interact over the course of their l...
Wolf–Rayet (WR) stars represent one of the final stages of massive stellar evolution. Relatively lit...
Context. Massive-binary evolution models predict that some systems will go through an evol...
© ESO, 2017. We present the first SB2 orbital solution and disentanglement of the massive Wolf-Raye...
Context. Most massive stars reside in multiple systems that will interact over the course of their l...
We present the results of an optical spectroscopic study of the massive Wolf-Rayet binary WR137. The...
Context. A significant number of the Wolf-Rayet stars seem to be binary or multiple systems, but the...
Computational models of Wolf-Rayet and other massive stars are presented at solar metallicity and at...