Visual Orbits of Wolf–Rayet Stars. I. The Orbit of the Dust-producing Wolf–Rayet Binary WR 137 Measured with the CHARA Array

• Published in: The Astrophysical journal Vol. 977; no. 1; pp. 78 - 90
• Main Authors: Richardson, Noel D., Schaefer, Gail H., Eldridge, Jan J., Spejcher, Rebecca, Holdsworth, Amanda, Lau, Ryan M., Monnier, John D., Moffat, Anthony F. J., Weigelt, Gerd, Williams, Peredur M., Kraus, Stefan, Le Bouquin, Jean-Baptiste, Anugu, Narsireddy, Chhabra, Sorabh, Codron, Isabelle, Ennis, Jacob, Gardner, Tyler, Gutierrez, Mayra, Ibrahim, Noura, Labdon, Aaron, Lanthermann, Cyprien, Setterholm, Benjamin R.
• Format: Journal Article
• Language: English
• Published: Philadelphia The American Astronomical Society 01.12.2024; IOP Publishing; American Astronomical Society
• Subjects: A stars; Angular resolution; Angular velocity; Arrays; Astronomical models; Astronomy; Binary stars; Companion stars; Dust; Dust formation; Helium; Hydrogen; Interferometric binary stars; Interferometry; Long baseline interferometry; Massive stars; O stars; Orbital elements; Sciences of the Universe; Stars; Stellar envelopes; Stellar winds; Visual observation; WC stars; Wolf-Rayet stars; WC stars; Long baseline interferometry; Dust formation; Wolf-Rayet stars; Interferometric binary stars; Astrophysics - Solar and Stellar Astrophysics
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ad8d5c

Classical Wolf–Rayet (W-R) stars are the descendants of massive OB stars that have lost their hydrogen envelopes and are burning helium in their cores prior to exploding as Type Ib/c supernovae. The mechanisms for losing their hydrogen envelopes are either through binary interactions or through strong stellar winds potentially coupled with episodic mass loss. Among the bright classical W-R stars, the binary system WR 137 (HD 192641; WC7d + O9e) is the subject of this paper. This binary is known to have a 13 yr period and produces dust near periastron. Here we report on interferometry with the Center for High Angular Resolution Astronomy Array collected over a decade of time and providing the first visual orbit for the system. We combine these astrometric measurements with archival radial velocities to measure masses of the stars of M WR = 9.5 ± 3.4 M ⊙ and M O = 17.3 ± 1.9 M ⊙ when we use the most recent Gaia distance. These results are then compared to predicted dust distribution using these orbital elements, which match the observed imaging from JWST as discussed recently by Lau et al. Furthermore, we compare the system to the Binary Population And Spectral Synthesis models, finding that the W-R star likely formed through stellar winds and not through binary interactions. However, the companion O star did likely accrete some material from the W-R star’s mass loss to provide the rotation seen today that drives its status as an Oe star.