Mass loss from late-type WN stars and itsZ-dependence

2008/03/06 by G. Gräfener, G. Graefener, W.‐R. Hamann +1 · 11 citations
Physics and Astronomy · #Astrophysical Phenomena and Observations #Gamma-ray bursts and supernovae #Stellar, planetary, and galactic studies #astro-ph

paper · pdf · doi:10.1051/0004-6361:20066176

16 pages, 10 figures, accepted by A&A

arxiv created 2008/03/06 · openalex publication_date 2008/03/11 · arxiv updated 2009/12/01 · openalex created_date 2022/08/31 · openalex updated_date 2026/07/30

Abstract

Context. The mass loss from Wolf-Rayet (WR) stars is of fundamental importance for the final fate of massive stars and their chemical yields. Its Z-dependence is discussed in relation to the formation of long-duration Gamma Ray Bursts (GRBs) and the yields from early stellar generations. However, the mechanism of formation of WR-type stellar winds is still under debate.

Citations

• Atomic data for opacity calculations. I. General description
• On the metallicity dependence of Wolf-Rayet winds
• First stars VI – Abundances of C, N, O, Li, and mixing in extremely metal-poor giants. Galactic evolution of the light elements
• Correcting for the Effects of Interstellar Extinction
• Stellar evolution with rotation

Cited by

• parsec evolutionary tracks of massive stars up to 350 M⊙at metallicities 0.0001 ≤Z≤ 0.04
• The very massive binary NGC 3603-A1
• Wind modelling of very massive stars up to 300 solar masses
• Low-metallicity massive single stars with rotation
• THE TRANSITION MASS-LOSS RATE: CALIBRATING THE ROLE OF LINE-DRIVEN WINDS IN MASSIVE STAR EVOLUTION
• Rotating Wolf-Rayet stars in a post RSG/LBV phase
• Intermediate mass black hole formation in compact young massive star clusters
• Creating and using large grids of precalculated model atmospheres for a rapid analysis of stellar spectra
• The Eddington factor as the key to understand the winds of the most massive stars. Evidence for a Γ-dependence of Wolf-Rayet type mass loss
• Global hot-star wind models for stars from Magellanic Clouds
• CAN THE SUBSONIC ACCRETION MODEL EXPLAIN THE SPIN PERIOD DISTRIBUTION OF WIND-FED X-RAY PULSARS?

Related

• A Conceptual Analysis of Mass Loss and Frequency Redistribution in Wolf-Rayet Winds
• On the metallicity dependence of Wolf-Rayet winds
• The Metallicity Dependence of Wolf-Rayet Mass Loss
• Peering into the Wolf-Rayet phenomenon through [WO] and [WC] stars
• The True origin of Wolf-Rayet stars