Scaled solar tracks and isochrones in a large region of the Z-Y plane. II. From 2.5 to 20 solar masses

By G. Bertelli, E. Nasi, L. Girardi, P. Observatory, A. Department, P. University. 2009

221 citations recorded by the source corpus.

We extend our theoretical computations for low-mass stars to intermediate-mass and massive stars, for which few databases exist in the literature. Evolutionary tracks and isochrones are computed for initial masses $2.50{-}20~M_{\odot}$ for a grid of 37 chemical compositions with metal content Z between 0.0001 and 0.070 and helium content Y between 0.23 and 0.40 to enable users to obtain isochrones for ages as young as about 10 7 years and to simulate stellar populations with different helium-to-metal enrichment laws. The Padova stellar evolution code is identical to that used in the first paper of this series. Synthetic TP-AGB models allow stellar tracks and isochrones to be extended until the end of the thermal pulses along the AGB. We provide software tools for the bidimensional interpolation (in Y and Z ) of the isochrones from very old ages down to about 10 7 years. This lower limit depends on chemical composition. The extension of the blue loops and the instability strip of Cepheid stars are compared and the Cepheid mass-discrepancy is discussed. The location of red supergiants in the H-R diagram is in good agreement with the evolutionary tracks for masses from 10 to $20~M_{\odot}$. Tracks and isochrones are available in tabular form for the adopted grid of chemical compositions in the extended plane $Z-Y$ in three photometric systems. An interactive web interface allows users to obtain isochrones of any chemical composition inside the provided $Z-Y$ range and also to simulate stellar populations with different $Y(Z)$ helium-to-metal enrichment laws.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/9fb7ecb17d3f9115625a490e7e6b587c105ac19b

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Citations in the corpus

A NEW GENERATION OF PARSEC-COLIBRI STELLAR ISOCHRONES INCLUDING THE TP-AGB PHASE (2017, result): “We also remark that similar TP-AGB sections are also found in the Bertelli et al. (2008, 2009) sets of isochrones.”
Mind Your Ps and Qs: The Interrelation between Period (P) and Mass-ratio (Q) Distributions of Binary Stars (2016, methodology): “Meanwhile, massive stars with M1 > 15M⊙ expand to much larger radii R1 = 700 - 1,200 R⊙ during their red supergiant phase (Bertelli et al. 2009).”
New constraints on the chemical evolution of the solar neighbourhood and galactic disc(s) - improved astrophysical parameters for the Geneva-Copenhagen Survey (2011, methodology): “In order to study differences between different isochrones, we used grids of the BASTI11 (Pietrinferni et al. 2004, 2006, 2009) and Padova12 isochrones (Bertelli et al. 2008, 2009).”
Gaia FGK benchmark stars: Effective temperatures and surface gravities (2015, methodology): “We selected the Padova stellar evolution models by Bertelli et al. (2008, 2009)10 and the Yonsei-Yale models by Yi et al. (2003), Demarque et al. (2004)11.”
New PARSEC evolutionary tracks of massive stars at low metallicity: testing canonical stellar evolution in nearby star-forming dwarf galaxies (2014, background): “…of stellar evolutionary tracks and isochrones has been continuously updated during the last decades (Girardi et al. 2002; Marigo et al. 2008; Bertelli et al. 2009), except for the models of the most massive stars (M >20 M ) that have remained untouched for two decades, after Bertelli et al.…”
parsec: stellar tracks and isochrones with the PAdova and TRieste Stellar Evolution Code (2012, methodology): “…the result of a thorough revision and update of the stellar evolution code used in Padova to compute sets of stellar evolutionary tr cks that are widely used by the astronomical community (Bressanet l. 1993; Bertelli et al. 1994; Girardi et al. 2000; Marigo et al.2001; Bertelli et al. 2008, 2009).”
BANYAN. XI. The BANYAN Σ Multivariate Bayesian Algorithm to Identify Members of Young Associations with 150 pc (2018, background): “In summary, thin disk stars are generated from a 3-slopes initial mass function and a decreasing star formation rate, and follow the evolutionary tracks of Bertelli et al. (1994, 2008, 2009) for masses larger than 0.7M , and from Chabrier & Baraffe (1997) for lower masses.”
PARSEC evolutionary tracks of massive stars up to 350 M ☉ at metallicities 0.0001 ≤ Z ≤ 0.04 (2015, background): “Since then, there have been many advances both in the basic input physics (opacities, equation of state, nuclear reactions) and in the mass-loss theory (and observations), and these called for a substantial revision of the Padova code.”
Galacticus: A Semi-Analytic Model of Galaxy Formation (2010, background): “Galacticus is supplied with a suitable file constructed from the tracks of Bertelli et al. (2008) and Bertelli et al. (2009).”
A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun (2010, methodology): “For main sequence and post-main sequence stars we used evolutionary models starting from the zero-age main sequence (ZAMS) from Schaller et al. (1992), Claret (2004), Pietrinferni et al. (2004)4, Bertelli et al. (2008, 2009) and Marques et al. (2008).”