Cover Image

Metal-poor single Wolf-Rayet stars: the interplay of optically thick winds and rotation

The Small Magellanic Cloud (SMC) hosts 12 known Wolf-Rayet (WR) stars, seven of which are apparently single. Their formation is a challenge for current stellar evolution models because line-driven winds are generally assumed to be quenched at a metallicity of Z ≤ 0.004. Here, we present a set of MES...

Full description

Saved in:
Bibliographic Details
Main Authors: Boco, Lumen (Author) , Mapelli, Michela (Author) , Sander, Andreas A. C. (Author) , Mesini, Sofia (Author) , Ramachandran, Varsha (Author) , Torniamenti, Stefano (Author) , Korb, Erika (Author) , Liu, Boyuan (Author) , Sabhahit, Gautham N. (Author) , Vink, Jorick S. (Author)
Format: Article (Journal)
Language:English
Published: 28 November 2025
In: Astronomy and astrophysics
Year: 2025, Volume: 703, Pages: 1-22
ISSN:1432-0746
DOI:10.1051/0004-6361/202556187
Online Access:Verlag, kostenfrei, Volltext: https://doi.org/10.1051/0004-6361/202556187
Verlag, kostenfrei, Volltext: https://www.aanda.org/articles/aa/abs/2025/11/aa56187-25/aa56187-25.html
Get full text
Author Notes:Lumen Boco, Michela Mapelli, Andreas A.C. Sander, Sofia Mesini, Varsha Ramachandran, Stefano Torniamenti, Erika Korb, Boyuan Liu, Gautham N. Sabhahit, and Jorick S. Vink
Description
Summary:The Small Magellanic Cloud (SMC) hosts 12 known Wolf-Rayet (WR) stars, seven of which are apparently single. Their formation is a challenge for current stellar evolution models because line-driven winds are generally assumed to be quenched at a metallicity of Z ≤ 0.004. Here, we present a set of MESA models of single stars with zero-age main sequence masses of 20 − 80 M⊙ considering different initial rotation speeds (Ω = 0 − 0.7 Ω c), metallicities (Z = 0.002 − 0.0045), and wind mass-loss models (optically thin and thick winds). We show that if we account for optically thick winds, fast rotating (Ω ∼ 0.6 Ω c) single metal-poor O-type stars (with M ≳ 20 M⊙) shed their envelope and become WR stars even at the low metallicity of the SMC. The luminosity, effective temperature, evolutionary timescale, surface abundance, and rotational velocity of our simulated WR stars are compatible to the WRs observed in the SMC. We speculate that this scenario can also alleviate the excess of giant stars across the Humphreys-Davidson limit. Our results have key implications for black hole masses, (pair instability) supernova explosions, and other observable signatures.
Item Description:Gesehen am 04.03.2026
Physical Description:Online Resource
ISSN:1432-0746
DOI:10.1051/0004-6361/202556187

Similar Items