PARSEC evolutionary tracks of massive stars up to 350 M ☉ at metallicities 0.0001 ≤ Z ≤ 0.04

  title={PARSEC evolutionary tracks of massive stars up to 350 M ☉ at metallicities 0.0001 ≤ Z ≤ 0.04},
  author={Yang Chen and Alessandro Bressan and L{\'e}o Girardi and Paola Marigo and Xu Kong and Antonio Lanza},
  journal={Monthly Notices of the Royal Astronomical Society},
We complement the PARSEC data base of stellar evolutionary tracks with new models of massive stars, from the pre-main sequence phase to the central carbon ignition. We consider a broad range of metallicities, 0.0001$\leq Z \leq$0.04 and initial masses up to $M_{\rm ini}=350\,M_\odot$. The main difference with respect to our previous models of massive stars is the adoption of a recent formalism accounting for the mass-loss enhancement when the ratio of the stellar to the Eddington luminosity… 

Figures from this paper

New parsec data base of α-enhanced stellar evolutionary tracks and isochrones – I. Calibration with 47 Tuc (NGC 104) and the improvement on RGB bump

Precise studies on the Galactic bulge, globular cluster, Galactic halo and Galactic thick disk require stellar models with alpha enhancement and various values of helium content. These models are

A bottom-heavy initial mass function for the likely-accreted blue-halo stars of the Milky Way

We use Gaia DR2 to measure the initial mass function (IMF) of stars within 250 pc and masses in the range 0.2 < m/M < 1.0, separated according to kinematics and metallicity, as determined from Gaia

Very massive stars, pair-instability supernovae and intermediate-mass black holes with the sevn code

Understanding the link between massive ($\gtrsim 30$ M$_{\odot{}}$) stellar black holes (BHs) and their progenitor stars is a crucial step to interpret observations of gravitational-wave events. In

A Fresh Look at AGB Stars in Galactic Open Clusters with Gaia: Impact on Stellar Models and the Initial–Final Mass Relation

Benefiting from the Gaia second and early third releases of photometric and astrometric data, we examine the population of asymptotic giant branch (AGB) stars that appear in the fields of

Massive black hole binaries from runaway collisions: the impact of metallicity

The runaway collision scenario is one of the most promising mechanisms to explain the formation of intermediate-mass black holes (IMBHs) in young dense star clusters. On the other hand, the massive

Testing models of stellar structure and evolution - I. Comparison with detached eclipsing binaries

We present the results of an analysis aimed at testing the accuracy and precision of the PARSEC v1.2S library of stellar evolution models, in a Bayesian framework, to infer stellar parameters. We

The effects of the initial mass function on Galactic chemical enrichment

Context. There is mounting evidence that the stellar initial mass function (IMF) could extend much beyond the canonical Mi ∼ 100M limit, but the impact of such hypothesis on the chemical enrichment

Ultraviolet spectra of extreme nearby star-forming regions: Evidence for an overabundance of very massive stars

As deep spectroscopic campaigns extend to higher redshifts and lower stellar masses, the interpretation of galaxy spectra depends increasingly upon models for very young stellar populations. Here we

ALMA observations of the nearby AGB star L2 Puppis - I. Mass of the central star and detection of a candidate planet

Six billion years from now, while evolving on the asymptotic giant branch (AGB), the Sun will metamorphose from a red giant into a beautiful planetary nebula. This spectacular evolution will impact


Thermally pulsing asymptotic giant branch (TP-AGB) stars are relatively short lived (less than a few Myr), yet their cool effective temperatures, high luminosities, efficient mass loss, and dust



New PARSEC evolutionary tracks of massive stars at low metallicity: testing canonical stellar evolution in nearby star-forming dwarf galaxies

We extend the {\sl\,PARSEC} library of stellar evolutionary tracks by computing new models of massive stars, from 14\Msun to 350\Msun. The input physics is the same used in the {\sl\,PARSEC}~V1.1

Evolutionary sequences of stellar models with new radiative opacities. VI. $Z=0.0001$

We present a large grid of stellar evolutionary models with the initial chemical composition (Z = 0:0001;Y =0 :23). These tracks are conceived to extend the grid of stellar models described 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 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

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

Rotating massive main-sequence stars - I. Grids of evolutionary models and isochrones

We present a dense grid of evolutionary tracks and isochrones of rotating massive main-sequence stars. We provide three grids with different initial compositions tailored to compare with early OB

Mass-loss predictions for evolved very metal-poor massive stars

Context. The first couple of stellar generations may have been massive, of order 100 M� , and to have played a dominant role in galaxy formation and the chemical enrichment of the early Universe.

Ionizing feedback from massive stars in massive clusters - III. Disruption of partially unbound clouds

We extend our previous SPH parameter study of the effects of photoionization from O-stars on star-forming clouds to include initially unbound clouds. We generate a set of model clouds in the mass

Improving PARSEC models for very low mass stars

Many stellar models present difficulties in reproducing basic observational relations of very low mass stars (VLMS), including the mass--radius relation and the optical colour--magnitudes of cool

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

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)