Implications of the metallicity dependence of Wolf-Rayet winds

@article{Eldridge2006ImplicationsOT,
  title={Implications of the metallicity dependence of Wolf-Rayet winds},
  author={J. J. Eldridge and Jorick S. Vink},
  journal={Astronomy and Astrophysics},
  year={2006},
  volume={452},
  pages={295-301}
}
Aims. Recent theoretical predictions for the winds of Wolf-Rayet stars indicate that their mass-loss rates scale with the initial stellar metallicity in the local Universe. We aim to investigate how this predicted dependence affects the models of Wolf-Rayet stars and their progeny in different chemical environments. Methods. We compute models of stellar structure and evolution for Wolf-Rayet stars for different initial metallicities, and investigate how the scaling of the Wolf-Rayet mass-loss… 

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References

SHOWING 1-10 OF 27 REFERENCES
Stellar evolution with rotation X: Wolf-Rayet star populations at solar metallicity
We examine the properties of Wolf-Rayet (WR) stars predicted by models of rotating stars taking account of the new mass loss rates for O-type stars and WR stars (Vink et al. 2000. 2001; Nugis &
Stellar evolution with rotation XI. Wolf-Rayet star populations at different metallicities
Grids of models of massive stars (M ≥ 20 M� ) with rotation are computed for metallicities Z ranging from that of the Small Magellanic Cloud (SMC) to that of the Galactic Centre. The hydrostatic
Stellar and wind properties of LMC WC4 stars A metallicity dependence for Wolf-Rayet mass-loss rates ?
We use ultraviolet space-based (FUSE, HST) and optical/IR ground-based (2.3 m MSSSO, NTT) spectroscopy to determine the physical parameters of six WC4-type Wolf-Rayet stars in the Large Magellanic
The effects of binaries on the evolution of Wolf-Rayet type spectral features in starbursts
In the present paper we investigate in detail the effects of binaries with initial period between 1 day and 10 years on theoretical simulations of Wolf-Rayet (WR) type spectral features in
On the relative frequencies of core-collapse supernovae sub-types: The role of progenitor metallicity
We show that the observed ratio N I b , c /N I I of the subtypes Ib,c and II core-collapse supernovae depends on the metallicity of the host galaxy, as expected on theoretical grounds. However, the
Which massive stars are gamma-ray burst progenitors?
The collapsar model for gamma-ray bursts requires three essential ingredients: a massive core, removal of the hydro- gen envelope, and enough angular momentum in the core. We study current massive
The distribution of low-mass stars in the Galactic disc
We quantify the complex interdependence of stellar binarity, the stellar mass-luminosity relation, the mass function, the colour-magnitude relation and Galactic disc structure, all of which must be
Mass-loss predictions for O and B stars as a function of metallicity
We have calculated a grid of massive star wind models and mass-loss rates for a wide range of metal abundances between 1=100 Z=Z 10. The calculation of this grid completes the Vink et al. (2000)
The progenitors of core-collapse supernovae
We present maps of the nature of single star progenitors of supernovae and their remnants in mass and metallicity space. We find our results are similar to others but we have gone further in varying
Stellar Evolution with Rotation
The existing grids of star models without rotation allow us to already explain a number of properties of massive and WR stars (cf. Maeder and Conti,1994). In particular, the sequences of star
...
...