Mass loss and the Eddington parameter: a new mass-loss recipe for hot and massive stars

  title={Mass loss and the Eddington parameter: a new mass-loss recipe for hot and massive stars},
  author={Joachim M. Bestenlehner},
  journal={Monthly Notices of the Royal Astronomical Society},
  • J. Bestenlehner
  • Published 12 February 2020
  • Physics
  • Monthly Notices of the Royal Astronomical Society
Mass loss through stellar winds plays a dominant role in the evolution of massive stars. In particular the mass-loss rates of very massive stars (VMSs, $> 100\,M_{\odot}$) are highly uncertain. Such stars display Wolf-Rayet spectral morphologies (WNh) whilst on the main-sequence. Metal-poor VMSs are progenitors of gamma-ray bursts and pair instability supernovae. In this study we extended the widely used stellar wind theory by Castor, Abbott & Klein from the optically thin (O star) to the… 

Figures and Tables from this paper

Physics and evolution of the most massive stars in 30 Doradus
The identification of stellar-mass black-hole mergers with up to 80 Msun as powerful sources of gravitational wave radiation led to increased interest in the physics of the most massive stars. The
The Uncertain Future of Massive Binaries Obscures the Origin of LIGO/Virgo Sources
The LIGO/Virgo gravitational-wave observatories have detected at least 50 double black hole (BH) coalescences. This sample is large enough to have allowed several recent studies to draw conclusions
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
On the nature of massive helium star winds and Wolf–Rayet-type mass-loss
The mass-loss rates of massive helium stars are one of the major uncertainties in modern astrophysics. Regardless of whether they were stripped by a binary companion or managed to peel off their
The R136 star cluster dissected with Hubble Space Telescope/STIS – II. Physical properties of the most massive stars in R136
We present an optical analysis of 55 members of R136, the central cluster in the Tarantula Nebula of the Large Magellanic Cloud. Our sample was observed with STIS aboard the Hubble Space Telescope,
pion: simulating bow shocks and circumstellar nebulae
Expanding nebulae are produced bymass loss from stars, especially during late stages of evolution.Multi-dimensional simulation of these nebulae requires high resolution near the star and permits
The changing-type SN 2014C may come from an 11-M⊙ star stripped by binary interaction and violent eruption
SN 2014C was an unprecedented supernova (SN) that displayed a metamorphosis from Type Ib to Type IIn over ∼200 days. This transformation is consistent with a helium star having exploded in a cavity


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
Mass loss from late-type WN stars and its Z-dependence: very massive stars approaching the Eddington limit
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
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
Context. The most massive stars are thought to be hydrogen-rich Wolf-Rayet stars of late spectral subtype (in the following WNh stars). The emission-line spectra of these stars are indicative of
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 VLT-FLAMES Tarantula Survey XVII. Physical and wind properties of massive stars at the top of the main sequence
The evolution and fate of very massive stars (VMS) is tightly connected to their mass-loss properties. Their initial and final masses differ significantly as a result of mass loss. VMS have strong
The transition mass-loss rate: Calibrating the role of line-driven winds in massive star evolution
A debate has arisen regarding the importance of stationary versus eruptive mass loss for massive star evolution. The reason is that stellar winds have been found to be clumped, which results in the
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
The Progenitor stars of gamma-ray bursts
Those massive stars that give rise to gamma-ray bursts (GRBs) during their deaths must be endowed with an unusually large amount of angular momentum in their inner regions, 1-2 orders of magnitude
New predictions for radiation-driven, steady-state mass-loss and wind-momentum from hot, massive stars
Context. Radiation-driven mass loss plays a key role in the life cycles of massive stars. However, basic predictions of such mass loss still suffer from significant quantitative uncertainties. Aims.
Evolution and fate of very massive stars
There is observational evidence that supports the existence of very massive stars (VMS) in the local universe. First, VMS (Mini ≲ 320 M⊙) have been observed in the Large Magellanic Clouds (LMC).