Mass-loss predictions for O and B stars as a function of metallicity

By J. Vink, A. D. Koter, Henny J.G.L.M. Lamers Astronomical Institute, Utrecht University, T. C. A. Institute, U. Amsterdam, T. Z. F. O. Science, Technology, Medicine, London and 1 more. 2001

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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) mass-loss recipe with an additional parameter Z. We have found that the exponent of the power law dependence of mass loss vs. metallicity is constant in the range between 1/30 Z=Z 3. The mass-loss rate scales as _ M / Z 0:85 v1 p with p = 1:23 for stars with Te > 25 000 K, and p = 1:60 for the B supergiants with Te 25 000 K, and _ M / Z 0:64 for B supergiants with Te < 25 000 K. Although it is derived that the exponent of the mass loss vs. metallicity dependence is constant over a large range in Z, one should be aware of the presence of bi-stability jumps at specic temperatures. Here the character of the line driving changes drastically due to recombinations of dominant metal species resulting in jumps in the mass loss. We have investigated the physical origins of these jumps and have derived formulae that combine mass loss recipes for both sides of such jumps. As observations of dierent galaxies show that the ratio Fe/O varies with metallicity, we make a distinction between the metal abundance Z derived on the basis of iron or oxygen lines. Our mass-loss predictions are successful in explaining the observed mass-loss rates for Galactic and Small Magellanic Cloud O- type stars, as well as in predicting the observed Galactic bi-stability jump. Hence, we believe that our predictions are reliable and suggest that our mass-loss recipe be used in future evolutionary calculations of massive stars at dierent metal abundance. A computer routine to calculate mass loss is publicly available.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/7761e535348ecc9aa15e5c7c0615f0781c1b6fa6

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Citations in the corpus

Physical Processes in the Interstellar Medium (2014, background): “The wind mass-loss rate scales somewhat less than quadratically with the stellar luminosity (e.g. Pauldrach & Puls, 1990; Puls et al., 1996; Vink et al., 2000, 2001), and as the luminosity L itself is a very steep function of stellar mass M , with L ∝M3.”
THE EFFECTS OF STELLAR ROTATION. II. A COMPREHENSIVE SET OF STARBURST99 MODELS (2014, background): “The v40-h and v00-h tracks adopt the theoretical rates of Vink et al. (2001) for ṀO.”
Rotating massive main-sequence stars - I. Grids of evolutionary models and isochrones (2011, methodology): “We updated the treatment of mass loss by stellar winds by implementing the prescription of Vink et al. (2000, 2001), based on the method by de Koter et al. (1997), for winds from early O- and B-type stars.”
Rotating massive main-sequence stars: II. Simulating a population of LMC early B-type stars as a test of rotational mixing (2011, methodology): “We use the recipe of Vink et al. (2000, 2001) for mass loss via stellar winds from O- and B-type stars.”
Mass loss from hot massive stars (2008, methodology): “Thereafter, efficient methods have been developed that allow for theoretical predictionsof mass-loss rates as a function of stellar parameters in the complete upper HRD (Vink et al 2000, 2001), and these can be used to check our standard picture of radiation-driven winds through comparison with empi”
Constraining Formation Models of Binary Black Holes with Gravitational-wave Observations (2017, background): “These include mass-loss prescriptions for O and B stars known as the “Vink prescription” (Vink et al. 2001), metallicity dependence to the evolution of Wolf-Rayet stars (Vink & de Koter 2005), and prescriptions for the supernova mechanism developed in Fryer et al. (2012).”
MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA) (2010, background): “…¨ ocker (1995) for AGB stars, de Jager et al. (1988) for a range of stars in the H-R diagram, mass loss for massive stars by Glebbeek et al. (2009), Vink et al. (2001), Nugis & Lamers (2000), and Nieuwenhuijzen & de Jager (1990), supersonic mass loss inspired by Prialnik & Kovetz (1995), and…”
The mass spectrum of compact remnants from the parsec stellar evolution tracks (2015, methodology): “In particular, we updated a version of SEBA that had been previously modiﬁed by Mapelli et al. (2013), who included metallicity-dependent stellar winds (Hurley, Pols & Tout 2000) and prescriptions for the mass loss by MS stars (Vink et al. 2001).”