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

被引:1
|
作者
Richardson, Noel D. [1 ]
Schaefer, Gail H. [2 ]
Eldridge, Jan J. [3 ]
Spejcher, Rebecca [1 ]
Holdsworth, Amanda [1 ]
Lau, Ryan M. [4 ]
Monnier, John D. [5 ]
Moffat, Anthony F. J. [6 ]
Weigelt, Gerd [7 ]
Williams, Peredur M. [8 ]
Kraus, Stefan [9 ]
Le Bouquin, Jean-Baptiste [10 ]
Anugu, Narsireddy [2 ]
Chhabra, Sorabh [9 ]
Codron, Isabelle [9 ]
Ennis, Jacob [5 ]
Gardner, Tyler [9 ]
Gutierrez, Mayra [5 ]
Ibrahim, Noura [5 ]
Labdon, Aaron [11 ]
Lanthermann, Cyprien [2 ]
Setterholm, Benjamin R. [5 ]
机构
[1] Embry Riddle Aeronaut Univ, Dept Phys & Astron, 3700 Willow Creek Rd, Prescott, AZ 86301 USA
[2] CHARA Array Georgia State Univ, Mt Wilson Observ, Mt Wilson, CA 91203 USA
[3] Univ Auckland, Dept Phys, Private Bag 92019, Auckland 1142, New Zealand
[4] NSFs NOIRLab, 950 N Cherry Ave, Tucson, AZ 85719 USA
[5] Univ Michigan, Astron Dept, Ann Arbor, MI 48109 USA
[6] Univ Montreal, Dept Phys, Complexe Sci,1375 Ave Therese Lavoie Roux, Montreal, PQ H2V 0B3, Canada
[7] MAX PLANCK INST RADIO ASTRON, BONN, Germany
[8] Royal Observ, Inst Astron, Edinburgh EH9 3HJ, Scotland
[9] Univ Coll Exeter, Exeter EX4 4QL, England
[10] Inst Planetol & Astrophys Grenoble, F-38058 Grenoble, France
[11] European Southern Observ, Casilla 19001, Santiago 19, Chile
来源
ASTROPHYSICAL JOURNAL | 2024年 / 977卷 / 01期
基金
美国国家科学基金会;
关键词
HIGH ANGULAR RESOLUTION; VIRTUAL OBSERVATORY TOOL; INTERACTING BINARIES; ECCENTRIC BINARY; SEARCHING CALIBRATORS; COLLIDING-WINDS; STELLAR MASSES; MASSIVE STARS; EVOLUTION; 1ST;
D O I
10.3847/1538-4357/ad8d5c
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
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 circle dot and M O = 17.3 +/- 1.9 M circle dot 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.
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页数:13
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