Helium stars: towards an understanding of Wolf–Rayet evolution

• Published in: Monthly notices of the Royal Astronomical Society Vol. 459; no. 2; pp. 1505 - 1518
• Main Authors: McClelland, L. A. S., Eldridge, J. J.
• Format: Journal Article
• Language: English
• Published: London Oxford University Press 21.06.2016
• Subjects: Astronomy; Helium; Massive stars; Mathematical models; Stars; Stars & galaxies; Stellar age; Stellar evolution; Supernovae; Temperature; Wind; stars: mass-loss; stars: massive; stars: Wolf–Rayet; stars: evolution; supernovae: general
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1093/mnras/stw618

Wolf–Rayet (WR) stars are massive stars that have lost most or all of their hydrogen via powerful stellar winds. Recent observations have indicated that hydrogen-free WR stars have cooler temperatures than those predicted by current evolutionary models. To investigate how varying mass-loss rate affects WR evolution, we have created a grid of pure helium star models. We compare our results with Galactic and Large Magellanic Cloud WR observations and show that the temperature ranges of observed WR stars can be reproduced by varying the mass-loss rate, which effectively determines the size of the helium envelope around the core. We also find that WN and WO stars arise from more massive stars, whereas WC stars come from lower masses. This contradicts the standard Conti scenario by which WN and WC stars evolve in an age sequence. We also predict the magnitudes of our models at core-collapse and compare with observations of nearby progenitors of Type Ib/c supernovae. We confirm the findings of previous studies that suggest WR stars are the progenitors of core-collapse supernovae; the progenitors would remain unobserved except in the cases where the progenitor is a low-mass helium giant, as is the case of iPTF13bvn.