A systematic study of super-Eddington layers in the envelopes of massive stars

Abstract

The proximity to the Eddington luminosity has been attributed as the cause of several observed effects in massive stars. Computationally, if the luminosity carried through radiation exceeds the local Eddington luminosity in the low-density envelopes of massive stars, it can result in numerical difficulties, inhibiting further computation of stellar models. This problem is exacerbated by the fact that very few massive stars are observed beyond the Humphreys-Davidson limit, the same region in the Hertzsprung-Russell diagram where the aforementioned numerical issues relating to the Eddington luminosity occur in stellar models. One-dimensional stellar evolution codes have to use pragmatic solutions to evolve massive stars through this computationally difficult phase. In this work, we quantify the impact of these solutions on the evolutionary properties of massive stars. We used the stellar evolution code MESA with commonly used input parameters for massive stellar models to compute the evolution of stars in the initial mass range of 10-110 M${}_{\odot }$ at one-tenth of solar metallicity. We find that numerical difficulties in stellar models with initial masses greater than or equal to 30 M${}_{\odot }$ cause these models to fail before the end of core helium burning. Recomputing these models using the same physical inputs but three different pragmatic solutions to treat the numerical instability, we find that the maximum radial expansion achieved by stars can vary by up to 2000 R${}_{\odot }$, while the remnant mass of the stars can vary by up to 14 M${}_{\odot }$ between the sets. These differences can have implications on studies such as binary population synthesis.

arXiv commentRevised version; Accepted for publication in A&A

References in corpus (73)

• Observation of Gravitational Waves from a Binary Black Hole Merger
• GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral
• The chemical composition of the Sun
• Modules for Experiments in Stellar Astrophysics (MESA)
• Modules for Experiments in Stellar Astrophysics (MESA): Giant Planets, Oscillations, Rotation, and Massive Stars
• Modules for Experiments in Stellar Astrophysics (MESA): Binaries, Pulsations, and Explosions
• MESA Isochrones and Stellar Tracks (MIST). I: Solar-Scaled Models
• Modules for Experiments in Stellar Astrophysics (MESA): Convective Boundaries, Element Diffusion, and Massive Star Explosions
• Modules for Experiments in Stellar Astrophysics (MESA): Pulsating Variable Stars, Rotation, Convective Boundaries, and Energy Conservation
• Mass-loss predictions for O and B stars as a function of metallicity
• Grids of stellar models with rotation - I. Models from 0.8 to 120 Msun at solar metallicity (Z = 0.014)
• Origin of the heavy elements in binary neutron-star mergers from a gravitational wave event
• Presupernova Evolution of Rotating Massive Stars I: Numerical Method and Evolution of the Internal Stellar Structure
• Mass Loss: Its Effect on the Evolution and Fate of High-Mass Stars
• Compact Remnant Mass Function: Dependence on the Explosion Mechanism and Metallicity
• Pre-Supernova Evolution of Massive Single and Binary Stars
• Rotating Massive Main-Sequence Stars I: Grids of Evolutionary Models and Isochrones
• Compact Object Modeling with the StarTrack Population Synthesis Code
• Black Hole Formation in Failing Core-Collapse Supernovae
• PARSEC evolutionary tracks of massive stars up to $350M_{\odot }$ at metallicities 0.0001$\le Z\le$0.04
• On The Maximum Mass of Stellar Black Holes
• On the metallicity dependence of Wolf-Rayet winds
• On the role of continuum-driven eruptions in the evolution of very massive stars and Population III stars
• A two-parameter criterion for classifying the explodability of massive stars by the neutrino-driven mechanism
• Formation of the first three gravitational-wave observations through isolated binary evolution
• Sub-surface convection zones in hot massive stars and their observable consequences
• The IACOB project: I. Rotational velocities in Northern Galactic O and early B-type stars revisited. The impact of other sources of line-broadening
• The Progenitors of Core-Collapse Supernovae
• The VLT-FLAMES Tarantula Survey I: Introduction and observational overview
• Mass loss from late-type WN stars and its Z-dependence: very massive stars approaching the Eddington limit
• The evolution of runaway stellar collision products
• A Porosity-Length Formalism for Photon-Tiring-Limited Mass Loss from Stars Above the Eddington Limit
• The Missing Luminous Blue Variables and the Bistability Jump
• Luminous Blue Variables are Antisocial: Their Isolation Implies that they are Kicked Mass Gainers in Binary Evolution
• A new mass-loss rate prescription for red supergiants
• Stellar envelope inflation near the Eddington limit. Implications for the radii of Wolf-Rayet stars and luminous blue variables
• The evolution of rotating very massive stars with LMC composition
• Massive main sequence stars evolving at the Eddington limit
• The temperatures of Red Supergiants
• Local Radiation Hydrodynamic Simulations of Massive Star Envelopes at the Iron Opacity Peak
• The VLT-FLAMES Tarantula Survey XVII. Physical and wind properties of massive stars at the top of the main sequence
• Hydrodynamic model atmospheres for WR stars: Self-consistent modeling of a WC star wind
• The IACOB project: III. New observational clues to understand macroturbulent broadening in massive O- and B-type stars
• A Systematic Survey of the Effects of Wind Mass Loss Algorithms on the Evolution of Single Massive Stars
• On Variations Of Pre-Supernova Model Properties
• New predictions for radiation-driven, steady-state mass-loss and wind-momentum from hot, massive stars II. A grid of O-type stars in the Galaxy and the Magellanic Clouds
• Constraining mixing in massive stars in the Small Magellanic Cloud
• Maximum Black Hole mass across Cosmic Time
• The luminosities of cool supergiants in the Magellanic Clouds, and the Humphreys-Davidson limit revisited
• Core-halo Structure of Chemically Homogeneous Massive Star and Bending of Zero-Age Main-Sequence
• Metallicity-dependent wind parameter predictions for OB stars
• Three Dimensional Radiation Hydrodynamic Simulations of Massive Star Envelopes
• Diverse Variability of O and B Stars Revealed from 2-minute Cadence Light Curves in Sectors 1 and 2 of the TESS Mission: Selection of an Asteroseismic Sample
• The metallicity dependence of envelope inflation in massive stars
• Impact of inter-correlated initial binary parameters on double black hole and neutron star mergers
• The fates of massive stars: exploring uncertainties in stellar evolution with METISSE
• Empirical mass-loss rates and clumping properties of Galactic early-type O supergiants
• The spectroscopic Hertzsprung-Russell diagram of hot massive stars in the SMC
• The excess of cool supergiants from contemporary stellar evolution models defies the metallicity-independent Humphreys-Davidson limit
• The Impact of Nuclear Reaction Rate Uncertainties On The Evolution of Core-Collapse Supernova Progenitors
• Stellar models with calibrated convection and temperature stratification from 3D hydrodynamics simulations
• Evolutionary models for R Coronae Borealis stars
• A theoretical investigation of the Humphreys-Davidson limit at high and low metallicity
• The theory of stellar winds
• Explaining the differences in massive star models from various simulations
• Instabilities in the Envelopes and Winds of Very Massive Stars
• Physics and evolution of the most massive stars in 30 Dor. Mass loss, envelope inflation, and a variable upper stellar mass limit
• Convectively Driven Three Dimensional Turbulence in Massive Star Envelopes: I. A 1D Implementation of Diffusive Radiative Transport
• Superadiabaticity and the metallicity independence of the Humphreys-Davidson limit
• Massive Star Evolution: Nucleosynthesis and Nuclear Reaction Rate Uncertainties
• 3D Simulations and MLT: I. Renzini's Critique
• Massive stellar models: rotational evolution, metallicity effects
• Neutrino cooling rates due to nickel isotopes for presupernova evolution of massive stars

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• Evolution of rotating massive stars adopting a newer, self-consistent wind prescription at SMC metallicity
• Collision-induced mass loss and mass gain on an extremely massive star. An analytical approach and a static proto-globular cluster test-case
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• Development of convective envelopes in massive stars: Implications for gravitational wave sources
• Hydrogen-free Wolf-Rayet stars: Helium stars with envelope-inflation structure and rotation
• Evolution of stars with 60 and 200 Msun: predictions for WNh stars in the Milky Way