Wolf-Rayet stars
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Massive Wolf-Rayet (WR) stars comprise a spectroscopic class characterized by high temperatures (Teff > ~30 kK) and powerful and rapid stellar winds. Hydrogen-rich WR stars represent the most massive stars in existence (M > ~100 Msun), while classical WR stars are hydrogen-depleted, evolved massive stars which probe the final evolutionary stages of massive stars prior to core collapse. They dominate entire stellar populations in terms of radiative and mechanical feedback, and are thought to give rise to powerful transients such as hydrogen-stripped supernovae (type Ibc SNe) and long-duration gamma-ray bursts (LGRBs). In this chapter, we summarize the main observed properties of WR populations in our Galaxy and nearby galaxies, and discuss open problems in our understanding of their structure and formation
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Cited by 2 Pith papers
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A Kinematic Study of Wolf-Rayet Stars at the Galactic Center I: Binary Candidates and Constraints on the Binary Fraction
30-year kinematic monitoring of 27 Galactic center Wolf-Rayet stars identifies five binary candidates and infers a binary fraction of 0.56 ± 0.18.
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A Rare Population of Intermediate-mass Helium Stars Between Hot Subdwarfs and Wolf-Rayet Stars
Binary population synthesis predicts several thousand intermediate-mass helium stars in the Milky Way, mostly in binaries, with metallicity and common-envelope ejection efficiency as the dominant shaping factors.
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