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

By Yang Chen, A. Bressan, L. Girardi, P. Marigo, X. Kong, A. Lanza. 2015

399 citations recorded by the source corpus.

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, $\Gamma_e$, approaches unity. With this new formalism, the models are able to reproduce the Humphreys-Davidson limit observed in the Galactic and Large Magellanic Cloud colour-magnitude diagrams, without an ad hoc mass-loss enhancement. We also follow the predictions of recent wind models indicating that the metallicity dependence of the mass-loss rates becomes shallower when $\Gamma_e$ approaches unity. We thus find that the more massive stars may suffer from substantial mass-loss even at low metallicity. We also predict that the Humphreys-Davidson limit should become brighter at decreasing metallicity. We supplement the evolutionary tracks with new tables of theoretical bolometric corrections, useful to compare tracks and isochrones with the observations. For this purpose, we homogenize existing stellar atmosphere libraries of hot and cool stars (PoWR, ATLAS9 and Phoenix) and we add, where needed, new atmosphere models computed with WM-basic. The mass, age and metallicity grids are fully adequate to perform detailed investigations of the properties of very young stellar systems, both in local and distant galaxies. The new tracks supersede the previous old Padova models of massive stars.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/22769f815c763cb6ce773613927adb5735b4da09

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Citations in the corpus

Massive black hole binaries from runaway collisions: the impact of metallicity (2016, methodology): “Moreover, the evolutionary models of massive and very massive stars have been deeply revised in the last few years (e.g. Vink et al. 2001; Vink & de Koter 2005; Yungelson et al. 2008; Tang et al. 2014; Chen et al. 2015 and references therein).”
The biggest splash (2019, methodology): “The data were compared to a grid of PARSEC isochrone models (Bressan et al. 2012; Chen et al. 2014; Tang et al. 2014; Chen et al. 2015) in a probabilistic sense.”
Merging black hole binaries with the SEVN code (2018, methodology): “The basic input physics is the same as that described in Bressan et al. (2012) and Chen et al. (2015), apart from the following small changes.”
Nuclear activity versus star formation: emission-line diagnostics at ultraviolet and optical wavelengths (2015, background): “The two stellar population spectra start to differ significantly at photon energies greater than 20 eV, the lowest-metallicity one being the hardest, as low-metallicity stars evolve at higher temperatures and luminosities than high-metallicity ones (e.g., Chen et al. 2015).”
COSMIC Variance in Binary Population Synthesis (2019, background): “…recent models suggest that as stars approach the limit imposed by the electron-scattering Eddington factor, Γe = χeL/(4πcGM) where χe is electron scattering opacity, winds may become insensitive to metallicity (e.g., Gräfener & Hamann 2008; Vink et al. 2011; Chen et al. 2015).”
Very massive stars, pair-instability supernovae and intermediate-mass black holes with the sevn code (2017, methodology): “We described an updated version of our population synthesis code, SEVN, where we included an analytical prescription for PPISNe and PISNe (derived from Woosley (2017)), and up-to-date stellar evolution tracks for VMSs, with MZAMS up to 350 M (Chen et al. 2015).”
Modelling the nebular emission from primeval to present-day star-forming galaxies (2016, methodology): “…over the past decade in the theories of stellar interiors (e.g., Eldridge et al. 2008; Bressan et al. 2012; Ekström et al. 2012; Georgy et al. 2013; Chen et al. 2015) and atmospheres (e.g., Hauschildt & Baron 1999; Hillier & Miller 1999; Pauldrach et al. 2001; Lanz & Hubeny 2003, 2007; Hamann &…”
The cosmic merger rate of neutron stars and black holes (2018, methodology): “In Mapelli et al. (2017), we estimate that the impact on the BHB merger rate of the difference between the Illustris mass-metallicity relation and the observational relation tent with PARSEC stellar evolution tracks (Chen et al. 2015) for stars with mass > 100 M , as discussed in Mapelli (2016).”
The progenitors of compact-object binaries: impact of metallicity, common envelope and natal kicks (2018, positive): “For all types of hot massive stars, we adopt a description of the mass loss as Ṁ ∝ Zβ , where Z is the metallicity and β = 0.85 if the Eddington ratio Γ < 2/3, β = 2.45−2.4Γ if 2/3≤ Γ < 1, and β = 0.05 if Γ≥ 1 (Chen et al. 2015).”
The cosmic merger rate of stellar black hole binaries from the Illustris simulation (2017, methodology): “Our BHBs were generated by evolving isolated stellar binaries with a new version of the BSE code (Hurley et al. 2002), which includes up-to-date recipes for stellar evolution and stellar winds (Vink et al. 2011; Chen et al. 2015).”
Merging black hole binaries: the effects of progenitor's metallicity, mass-loss rate and Eddington factor (2017, methodology): “…stellar evolution is implemented using polynomial fitting formulas (Hurley et al. 2000), while in SEVN stellar evolution is calculated from look-up tables (the current default tables are based on the recent PARSEC stellar evolution code, Bressan et al. 2012; Tang et al. 2014; Chen et al. 2015).”
The effect of pair-instability mass loss on black-hole mergers (2016, methodology): “More advanced stellar models are now available (e.g. Chen et al. 2015) and some include effects of rotation on stellar evolution (Georgy et al. 2013; Choi et al. 2016).”
Pulsational Pair-instability Supernovae (2016, background): “Other recent theoretical studies (e.g., Chen et al. 2015) also show stars with 10% solar metallicity and masses up to 150 M ending their lives as RSG’s.”
The Lives of Stars: Insights from the TGAS–RAVE–LAMOST Data Set (2018, methodology): “An isochrone grid is constructed using the Padova isochrones4 (see Bressan et al. 2012, Chen et al. 2014, Chen et al. 2015, Tang et al. 2014).”
A NEW GENERATION OF PARSEC-COLIBRI STELLAR ISOCHRONES INCLUDING THE TP-AGB PHASE (2017, background): “Such massive star models are described in Tang et al. (2014) and Chen et al. (2015), to whom we refer for all details.”
Merging black holes in young star clusters (2019, methodology): “MOBSE implements some of the most recent stellar wind models for massive hot stars (Vink et al. 2001; Gräfener & Hamann 2008; Vink et al. 2011; Vink 2016), including the impact of the Eddington factor Γe on mass loss (Gräfener & Hamann 2008; Chen et al. 2015).”