Metallicity-dependent wind parameter predictions for OB stars

  title={Metallicity-dependent wind parameter predictions for OB stars},
  author={Jorick S. Vink and Andreas A. C. Sander},
Mass-loss rates and terminal wind velocities are key parameters that determine the kinetic wind energy and momenta of massive stars. Furthermore, accurate mass-loss rates determine the mass and rotational velocity evolution of mass stars, and their fates as neutron stars and black holes in function of metallicity (Z). Here we update our Monte Carlo mass-loss Recipe with new dynamically-consistent computations of the terminal wind velocity – as a function of Z . These predictions are… 
Far-ultraviolet Spectra of Main-sequence O Stars at Extremely Low Metallicity
Metal-poor massive stars dominate the light we observe from star-forming dwarf galaxies and may have produced the bulk of energetic photons that reionized the universe at high redshift. Yet, the
Detectability of Population III stellar remnants as X-ray binaries from tidal captures in the local Universe
We assess the feasibility of detecting the compact object remnants from Population III (Pop III) stars in nearby dense star clusters, where they become luminous again as X-ray binaries (XRBs) and
Star Formation Regulation and Self-pollution by Stellar Wind Feedback
Stellar winds contain enough energy to easily disrupt the parent cloud surrounding a nascent star cluster, and for this reason they have long been considered candidates for regulating star formation.
Binary Black Hole Formation with Detailed Modeling: Stable Mass Transfer Leads to Lower Merger Rates
Rapid binary population synthesis codes are often used to investigate the evolution of compact-object binaries. They typically rely on analytical fits of single-star evolutionary tracks and
X-ray emission from BH+O star binaries expected to descend from the observed galactic WR+O binaries
In the Milky Way, $\sim$18 Wolf-Rayet+O (WR+O) binaries are known with estimates of their stellar and orbital parameters. Whereas black hole+O (BH+O) binaries are thought to evolve from the former,
Superluminous supernovae: an explosive decade
Ten years on from the discovery of mysterious events 100 times brighter than conventional stellar explosions, Matt Nicholl charts our understanding of superluminous supernovae


Predictions for mass-loss rates and terminal wind velocities of massive O-type stars
Context. Mass loss from massive stars forms an important aspect of the evolution of massive stars, as well as for the enrichment of the surrounding interstellar medium. Aims. Our goal is to predict
Mass loss from hot massive stars
Mass loss is a key process in the evolution of massive stars, and must be understood quantitatively if it is to be successfully included in broader astrophysical applications such as galactic and
Driving classical Wolf-Rayet winds: A Γ- and Z-dependent mass-loss
Classical Wolf-Rayet (WR) stars are at a crucial evolutionary stage for constraining the fates of massive stars. The feedback of these hot, hydrogen-depleted stars dominates their surrounding by
The empirical metallicity dependence of the mass-loss rate of O- and early B-type stars
We present a comprehensive study of the observational dependence of the mass-loss rate in stationary stellar winds of hot massive stars on the metal content of their atmospheres. The metal content of
Line-driven Winds, Ionizing Fluxes, and Ultraviolet Spectra of Hot Stars at Extremely Low Metallicity. I. Very Massive O Stars
Wind models of very massive stars with metallicities in a range from 10-4 to 1.0 solar are calculated using a new treatment of radiation-driven winds with depth-dependent radiative force multipliers
CMF models of hot star winds II. Reduction of O star wind mass-loss rates in global models
We calculate global (unified) wind models of main-sequence, giant, and supergiant O stars from our Galaxy. The models are calculated by solving hydrodynamic, kinetic equilibrium (also known as NLTE)
Implications of the metallicity dependence of Wolf-Rayet winds
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
Wind modelling of very massive stars up to 300 solar masses
The stellar upper-mass limit is highly uncertain. Some studies have claimed there is a universal upper limit of ∼150 M� . A factor that is often overlooked is that there might be a significant
Testing the predicted mass-loss bi-stability jump at radio wavelengths
Context. Massive stars play a dominant role in the Universe, but one of the main drivers for their evolution, their mass loss, remains poorly understood. Aims. In this study, we test the
Two bi-stability jumps in theoretical wind models for massive stars and the implications for luminous blue variable supernovae
Luminous Blue Variables have been suggested to be the direct progenitors of supernova types IIb and IIn, with enhanced mass loss prior to explosion. However, the mechanism of this mass loss is not