Visual Orbits of Wolf-Rayet Stars II: The Orbit of the Nitrogen-Rich WR Binary WR 138 measured with the CHARA Array
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| Format: | Preprint |
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2024
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| author | Holdsworth, Amanda Richardson, Noel Schaefer, Gail H. Eldridge, Jan J. Hill, Grant M. Spejcher, Becca Mackey, Jonathan Moffat, Anthony F. J. Navarete, Felipe Monnier, John D. Kraus, Stefan Bouquin, Jean-Baptiste Le Anugu, Narsireddy Chhabra, Sorabh Codron, Isabelle Ennis, Jacob Gardner, Tyler Gutierrez, Mayra Ibrahim, Noura Labdon, Aaron Lanthermann, Cyprien Setterholm, Benjamin R. |
| author_facet | Holdsworth, Amanda Richardson, Noel Schaefer, Gail H. Eldridge, Jan J. Hill, Grant M. Spejcher, Becca Mackey, Jonathan Moffat, Anthony F. J. Navarete, Felipe Monnier, John D. Kraus, Stefan Bouquin, Jean-Baptiste Le Anugu, Narsireddy Chhabra, Sorabh Codron, Isabelle Ennis, Jacob Gardner, Tyler Gutierrez, Mayra Ibrahim, Noura Labdon, Aaron Lanthermann, Cyprien Setterholm, Benjamin R. |
| contents | Classical Wolf-Rayet stars are descendants of massive OB-type stars that have lost their hydrogen-rich envelopes, and are in the final stages of stellar evolution, possibly exploding as type Ib/c supernovae. It is understood that the mechanisms driving this mass-loss are either strong stellar winds and or binary interactions, so intense studies of these binaries including their evolution can tell us about the importance of the two pathways in WR formation. WR 138 (HD 193077) has a period of just over 4 years and was previously reported to be resolved through interferometry. We report on new interferometric data combined with spectroscopic radial velocities in order to provide a three-dimensional orbit of the system. The precision on our parameters tend to be about an order of magnitude better than previous spectroscopic techniques. These measurements provide masses of the stars, namely $M_{\rm WR} = 13.93\pm1.49M_{\odot}$ and $M_{\rm O} = 26.28\pm1.71M_{\odot}$. The derived orbital parallax agrees with the parallax from \textit{Gaia}, namely with a distance of 2.13 kpc. We compare the system's orbit to models from BPASS, showing that the system likely may have been formed with little interaction but could have formed through some binary interactions either following or at the start of a red supergiant phase, but with the most likely scenario occurring as the red supergiant phase starts for a $\sim 40M_\odot$ star. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2411_01062 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Visual Orbits of Wolf-Rayet Stars II: The Orbit of the Nitrogen-Rich WR Binary WR 138 measured with the CHARA Array Holdsworth, Amanda Richardson, Noel Schaefer, Gail H. Eldridge, Jan J. Hill, Grant M. Spejcher, Becca Mackey, Jonathan Moffat, Anthony F. J. Navarete, Felipe Monnier, John D. Kraus, Stefan Bouquin, Jean-Baptiste Le Anugu, Narsireddy Chhabra, Sorabh Codron, Isabelle Ennis, Jacob Gardner, Tyler Gutierrez, Mayra Ibrahim, Noura Labdon, Aaron Lanthermann, Cyprien Setterholm, Benjamin R. Solar and Stellar Astrophysics Classical Wolf-Rayet stars are descendants of massive OB-type stars that have lost their hydrogen-rich envelopes, and are in the final stages of stellar evolution, possibly exploding as type Ib/c supernovae. It is understood that the mechanisms driving this mass-loss are either strong stellar winds and or binary interactions, so intense studies of these binaries including their evolution can tell us about the importance of the two pathways in WR formation. WR 138 (HD 193077) has a period of just over 4 years and was previously reported to be resolved through interferometry. We report on new interferometric data combined with spectroscopic radial velocities in order to provide a three-dimensional orbit of the system. The precision on our parameters tend to be about an order of magnitude better than previous spectroscopic techniques. These measurements provide masses of the stars, namely $M_{\rm WR} = 13.93\pm1.49M_{\odot}$ and $M_{\rm O} = 26.28\pm1.71M_{\odot}$. The derived orbital parallax agrees with the parallax from \textit{Gaia}, namely with a distance of 2.13 kpc. We compare the system's orbit to models from BPASS, showing that the system likely may have been formed with little interaction but could have formed through some binary interactions either following or at the start of a red supergiant phase, but with the most likely scenario occurring as the red supergiant phase starts for a $\sim 40M_\odot$ star. |
| title | Visual Orbits of Wolf-Rayet Stars II: The Orbit of the Nitrogen-Rich WR Binary WR 138 measured with the CHARA Array |
| topic | Solar and Stellar Astrophysics |
| url | https://arxiv.org/abs/2411.01062 |