Article Dans Une Revue The Astrophysical Journal Année : 2024

Visual Orbits of Wolf–Rayet Stars. II. The Orbit of the Nitrogen-rich Wolf–Rayet Binary WR 138 Measured with the CHARA Array

Amanda Holdsworth
Noel Richardson
Gail H Schaefer
Jan J Eldridge
Grant M Hill
Becca Spejcher
  • Fonction : Auteur
Jonathan Mackey
Anthony F J Moffat
Felipe Navarete
  • Fonction : Auteur
John D Monnier
Stefan Kraus
  • Fonction : Auteur
Narsireddy Anugu
  • Fonction : Auteur
Sorabh Chhabra
  • Fonction : Auteur
Isabelle Codron
  • Fonction : Auteur
Jacob Ennis
  • Fonction : Auteur
Tyler Gardner
  • Fonction : Auteur
Mayra Gutierrez
  • Fonction : Auteur
Noura Ibrahim
  • Fonction : Auteur
Aaron Labdon
  • Fonction : Auteur
Cyprien Lanthermann
  • Fonction : Auteur
Benjamin R Setterholm
  • Fonction : Auteur

Résumé

Classical Wolf–Rayet (WR) 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 yr 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 WR = 13.93 ± 1.49 M ⊙ and M O = 26.28 ± 1.71 M ⊙ . The derived orbital parallax agrees with the parallax from 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 ∼40 M ⊙ star.
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hal-04959282 , version 1 (20-02-2025)

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Amanda Holdsworth, Noel Richardson, Gail H Schaefer, Jan J Eldridge, Grant M Hill, et al.. Visual Orbits of Wolf–Rayet Stars. II. The Orbit of the Nitrogen-rich Wolf–Rayet Binary WR 138 Measured with the CHARA Array. The Astrophysical Journal, 2024, 977 (2), pp.185. ⟨10.3847/1538-4357/ad9024⟩. ⟨hal-04959282⟩
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