Scaled solar tracks and isochrones in a large region of the Z-Y plane I. From the ZAMS to the TP-A

By G. Bertelli, L. Girardi, P. Marigo, E. I. Observatory, A. Department, P. University. 2008

325 citations recorded by the source corpus.

Context. In many astrophysical contexts, the helium content of stars may differ significantly from those usually assumed in evolution- ary calculations. Aims. In order to improve upon this situation, we have computed tracks and isochrones in the range of initial masses 0.15−20 Mfor a grid of 39 chemical compositions with the metal content Z between 0.0001 and 0.070 and helium content Y between 0.23 and 0.46. Methods. The Padova stellar evolution code has been implemented with updated physics. New synthetic TP-AGB models allow the extension of stellar models and isochrones until the end of the thermal pulses along the AGB. Software tools for the bidimensional interpolation (in Y and Z) of the tracks have been tuned. Results. This first paper presents tracks for low mass stars (from 0.15 to 2.5 M� ) with scaled-solar abundances and the corresponding isochrones from very old ages down to about 1 Gyr. Conclusions. Tracks and isochrones are made available in tabular form for the adopted grid of chemical compositions in the plane Z-Y. As soon as possible an interactive web interface will allow users to obtain isochrones of any chemical composition and also simulated stellar populations with different Y(Z) helium-to-metal enrichment laws.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/ce872dfad92d0d611f15a3528ba3ea145590b919

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

Citations in the corpus

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).”
Kinematics and history of the solar neighbourhood revisited (2009, methodology): “Bertelli et al. (2008) argue that the update of the solar chemical composition by Grevesse, Asplund & Sauval (2007) (Y = 0.2486, Z = 0.0122) gives rise to several problems and uncertainties and adopt (Y = 0.260, Z = 0.017) for their solar model.”
Fundamental parameters and infrared excesses of Hipparcos stars (2012, methodology): “As a cursory analysis, we present solar-metallicity Padova isochrones (Bertelli et al. 2008; Marigo et al. 2008) for a variety of ages in Fig.”
SPIDER VIII - constraints on the stellar initial mass function of early-type galaxies from a variety of spectral features (2013, methodology): “To generate stellar spectra, we use the Padova evolutionary tracks (Bertelli et al. 2008), identifying 16 log g– Teff pairs along the 12Gyr isochrone, from the tip of the RGB (Teff = 3000K and log g = −0.1) down to the main sequence locus corresponding to a stellar mass of 0.15M⊙ (Teff = 3400K and…”
Luminosities and mass-loss rates of SMC and LMC AGB stars and red supergiants (2009, background): “Figure 9 shows the Hertzsprung-Russell diagram with evolutionary tracks of Bertelli et al. (2008), extended to unpublished tracks of more massive stars (Girardi, priv. comm.) forZ= 0.008.”
On the α formalism for the common envelope interaction (2010, methodology): “The second set is from the computations of Bertelli et al. (2008), who calculated an extensive grid of models including their metallicity dependence.”
The Gemini Planet Imager Exoplanet Survey: Giant Planet and Brown Dwarf Demographics from 10 to 100 au (2019, methodology): “…values used in these analyses, with the Siess et al. (2000) models used by Nielsen et al. (2013) assuming a solar metallicity of Ze=0.02, David & Hillenbrand (2015) using the PARSEC model grid which assumes Ze=0.0152, while Mamajek (2012) used a Ze= 0.017 and the Bertelli et al. (2008) model grid.”
The second and third parameters of the horizontal branch in globular clusters (2010, methodology): “We estimated this expected colour spread in the MS at absolute magnitude MV = +8, by using the following formulae we derived by fitting data from the Bertelli et al. (2008) isochrones δ(B − V) = δY(0.350− 0.035[Fe/H]) (16) and δ(V − I) = δY(0.672+ 0.099[Fe/H]).”
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).”
A NEW GENERATION OF PARSEC-COLIBRI STELLAR ISOCHRONES INCLUDING THE TP-AGB PHASE (2017, methodology): “We also remark that similar TP-AGB sections are also found in the Bertelli et al. (2008, 2009) sets of isochrones.”
The GALAH survey: observational overview and Gaia DR1 companion (2016, methodology): “Absolute magnitudes in Johnson V and 2MASS J bands are estimated from theoretical Padova isochrones (Bertelli et al. 2008) with weights determined (as described in Zwitter et al. 2010) using a mass function from Chabrier (2003), a flat prior on ages between 0.5 and 12 Gyr and a flat prior on space…”
parsec: stellar tracks and isochrones with the PAdova and TRieste Stellar Evolution Code (2012, methodology): “At variance with previous releases (Bressan et al. 1993; Girardi et al. 2000; Bertelli et al. 2008), where the limiting masses MO1 and MO2 were fixed (MO1 = 1 M⊙ and MO2 = 1.5 M⊙), we now adopt a transition region that depends on the initial chemical composition of the model set.”
Asteroseismology of old open clusters with Kepler: direct estimate of the integrated red giant branch mass-loss in NGC 6791 and 6819 (2011, methodology): “We now compare the difference between the average mass of low-luminosity RGB and RC stars to theoretical predictions using a revised version of the YZVAR1 isochrones and stellar evolutionary sequences (Bertelli et al. 2008; Bertelli 1 http://stev.oapd.inaf.it/YZVAR/ 2011, private communication).”
Constraining the thick disc formation scenario of the Milky Way (2014, unknown): “We alternatively attempted to use Padova isochrones (Bertelli et al. 2008).”
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).”
Scaled solar tracks and isochrones in a large region of the Z-Y plane. II. From 2.5 to 20 solar masses (2009, methodology): “We adopt the same prescription as in Paper I (Bertelli et al. 2008) and in Girardi et al. (2000) for the parameterΛc for H- and He-burning stages.”