Evolution of rotating massive stars with new hydrodynamic wind models

Abstract

Mass loss due to line-driven winds is central to our understanding of the evolution of massive stars. We extend the evolution models introduced in Paper I, where the mass loss recipe is based on the simultaneous calculation of the wind hydrodynamics and the line-acceleration, by incorporating the effects of stellar rotation. We introduce a grid of self-consistent line-force parameters for a set of standard evolutionary tracks. With that, we generate a new set of evolutionary tracks with rotation for $M_{\text{ZAMS}}=25,40,70,$ and $120M_{\odot }$, and metallicities $Z=0.014$ and $0.006$. The self-consistent approach gives lower mass loss rates than the standard values adopted in previous evolution models. This decrease impacts strongly on the tracks of the most massive models. Weaker winds allow the star to retain more mass, but also more angular momentum. As a consequence, weaker wind models rotate faster and show a less efficient mixing in their inner stellar structure. The new tracks predict an evolution of the rotational velocities through the MS in close agreement with the range of $\varv\sin i$ values found by recent surveys of Galactic O-type stars. As subsequent implications, the weaker winds from self-consistent models suggest a reduction of the contribution of the isotope ${}^{26}$Al to the ISM due to stellar winds of massive stars during the MS phase. Moreover, the higher luminosities found for the self-consistent evolutionary models suggest that some populations of massive stars might be less massive than previously thought, as in the case of Ofpe stars at the Galactic Centre. Therefore, this study opens a wide range of consequences for further research based on the evolution of massive stars.

arXiv commentAccepted for publication in Astronomy & Astrophysics journal

References in corpus (68)

• The chemical composition of the Sun
• How Massive Single Stars End their Life
• 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)
• The Galactic Center Massive Black Hole and Nuclear Star Cluster
• Rotating Massive Main-Sequence Stars I: Grids of Evolutionary Models and Isochrones
• Astrophysical Implications of the Binary Black-Hole Merger GW150914
• Radioactive 26Al and massive stars in the Galaxy
• On The Maximum Mass of Stellar Black Holes
• The R136 star cluster hosts several stars whose individual masses greatly exceed the accepted 150 Msun stellar mass limit
• The rotation rates of massive stars: the role of binary interaction through tides, mass transfer and mergers
• First Sagittarius A* Event Horizon Telescope Results. V. Testing Astrophysical Models of the Galactic Center Black Hole
• Stellar evolution with rotation XI: Wolf-Rayet star populations at different metallicities
• Single star progenitors of long gamma-ray bursts I: Model grids and redshift dependent GRB rate
• Grids of stellar models with rotation - III. Models from 0.8 to 120 Msun at a metallicity Z = 0.002
• The Galactic WN stars: Spectral analyses with line-blanketed model atmospheres versus stellar evolution models with and without rotation
• Stellar Populations in the Central 0.5 pc of the Galaxy II: The Initial Mass Function
• Evolution and fate of very massive stars
• Mass loss from late-type WN stars and its Z-dependence: very massive stars approaching the Eddington limit
• Evolution towards the critical limit and the origin of Be stars
• Stellar and wind properties of massive stars in the central parsec of the Galaxy
• Properties of Galactic early-type O-supergiants: A combined FUV-UV and optical analysis
• The spectroscopic Hertzsprung-Russell diagram
• The evolution of massive stars and their spectra I. A non-rotating 60 Msun star from the zero-age main sequence to the pre-supernova stage
• The VLT-FLAMES Tarantula Survey XVII. Physical and wind properties of massive stars at the top of the main sequence
• Low-metallicity massive single stars with rotation. Evolutionary models applicable to I Zwicky 18
• Variable accretion and emission from the stellar winds in the Galactic centre
• 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
• Twelve years of spectroscopic monitoring in the Galactic Center: the closest look at S-stars near the black hole
• Theory and Diagnostics of Hot Star Mass Loss
• Hydrodynamic Simulations of the Inner Accretion Flow of Sagittarius A* Fueled By Stellar Winds
• Macroclumping as solution of the discrepancy between Hα and P v mass loss diagnostics for O-type stars
• The IACOB project. V. Spectroscopic parameters of the O-type stars in the modern grid of standards for spectral classification
• New estimates of the contribution of Wolf--Rayet stellar winds to the Galactic 26Al
• The Surprisingly Small Impact of Magnetic Fields On The Inner Accretion Flow of Sagittarius A* Fueled By Stellar Winds
• The influence of rotation in radiation driven wind from hot stars: New solutions and disk formation in Be stars
• Effects of close binary evolution on the main-sequence morphology of young star clusters
• Spectral and intensity variations of Galactic 26^Al emission
• The young stars in the Galactic Center
• Accretion of cool stellar winds on Sgr A*: another puzzle of the Galactic Centre?
• Grids of stellar models with rotation VI: Models from 0.8 to 120 $M_{\odot }$ at a metallicity Z = 0.006
• Effects of anisotropic winds on massive stars evolution
• The puzzle of the CNO abundances of α Cygni variables resolved by the Ledoux criterion?
• The IACOB project. VII. The rotational properties of Galactic massive O-type stars revisited
• Modeling the early evolution of massive OB stars with an experimental wind routine
• The IACOB project. VI. On the elusive detection of massive O-type stars close to the ZAMS
• Convective core sizes in rotating massive stars: I. Constraints from solar metallicity OB field stars
• Stellar winds pump the heart of the Milky Way
• Spectroscopic evolution of very massive stars at Z = 1/2.5 Zsun
• Explaining the differences in massive star models from various simulations
• Clump formation through colliding stellar winds in the Galactic Centre
• Physics and evolution of the most massive stars in 30 Dor. Mass loss, envelope inflation, and a variable upper stellar mass limit
• The role of feedback in accretion on Low Luminosity AGN: Sgr A* case study
• Global hot-star wind models for stars from Magellanic Clouds
• 3D simulations of clump formation in stellar wind collisions
• Self-consistent modelling of line-driven hot-star winds with Monte Carlo radiation hydrodynamics
• Comparing simulated ${}^{26}$Al maps to gamma-ray measurements
• An Updated Formalism For Line-Driven Radiative Acceleration and Implications for Stellar Mass Loss
• Evolution of massive stars with new hydrodynamic wind models
• Self-consistent solutions for line-driven winds of hot massive stars. The m-CAK procedure
• Method and new tabulations for flux-weighted line-opacity and radiation line-force in supersonic media
• Very massive star winds as sources of the short-lived radioactive isotope ${}^{26}$Al
• The hydrogen clock to infer the upper stellar mass
• New self-consistent wind parameters fitting optical spectra of O-type stars observed with HERMES spectrograph
• A New Numerical Method for Solving Radiation Driven Winds from Hot Stars
• Co-existence and switching between fast and $\Omega$-slow wind solutions in rapidly rotating massive stars
• $\Omega$-Slow Solutions and Be Star Disks

Cited by in corpus (9)

• Extreme N-emitters at high-redshift: signatures of supermassive stars and globular cluster or black hole formation in action?
• Very Massive Star Models: I. Impact of Rotation and Metallicity and Comparisons with Observations
• Tracing the evolution of short-period binaries with super-synchronous fast rotators
• Evolution of rotating massive stars adopting a newer, self-consistent wind prescription at SMC metallicity
• The formation and stability of a cold disc made out of stellar winds in the Galactic Centre
• Exploring extreme brightness variations in blue supergiant MACHO 80.7443.1718: Evidence for companion-driven enhanced mass loss
• Evolution of stars with 60 and 200 Msun: predictions for WNh stars in the Milky Way
• Asymmetric emissions of neutrinos in the cooling of rotating proto-neutron stars
• Revisiting the Evolutionary Status of Massive Stars at the central parsec of the Milky Way