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

Abstract 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.

Authors

Publication Details

Journal
The Astrophysical Journal
Published
2024-12-01
DOI
https://doi.org/10.3847/1538-4357/ad8d5c
Citations
6
Primary Topic
Stellar, planetary, and galactic studies
Type
article
Field-Weighted Citation Impact
1.99

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article

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

Cyprien Lanthermann, Gail H. Schaefer, Sorabh Chhabra, Mayra Gutierrez et al.
6 citations
The Astrophysical Journal
Stellar, planetary, and galactic studies
1.99
article

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

Cyprien Lanthermann, Gail H. Schaefer, Sorabh Chhabra, Mayra Gutierrez, John D. Monnier, P. M. Williams, Benjamin R. Setterholm, Ryan M. Lau, A. F. J. Moffat, Stefan Kraus, Narsireddy Anugu, Aaron Labdon, G. Weigelt, Jacob Ennis, Noel D. Richardson, Tyler Gardner, Noura Ibrahim, J. J. Eldridge, Isabelle Codron, Jean-Baptiste Le Bouquin, Rebecca Spejcher, Amanda Holdsworth
article en
6 citations

Abstract

Abstract 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.

The Astrophysical JournalVol. 977(1)
National Science Foundation, National Aeronautics and Space Administration, Research Corporation for Science Advancement, Georgia State University, European Commission, Horizon 2020 Framework Programme, Office of the Vice President for Research and Economic Development, University at Buffalo
Openalex Percentile: Top 14%
Stellar, planetary, and galactic studies
1.99
DOIOpen Access PDFOpenAlex
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