A Large Stellar Evolution Database for Population Synthesis Studies. I. Scaled Solar Models and Isochrones

By Adriano Pietrinferni, Santi Cassisi, Maurizio Salaris, Fiorella Castelli. 2004

1,073 citations recorded by the source corpus.

We present a large and updated stellar evolution database for low-, intermediate-, and high-mass stars in a wide metallicity range, suitable for studying Galactic and extragalactic simple and composite stellar populations using population synthesis techniques. The stellar mass range is between ~0.5 and 10 M☉ with a fine mass spacing. The metallicity [Fe/H] comprises 10 values ranging from -2.27 to 0.40, with a scaled solar metal distribution. The initial He mass fraction ranges from Y = 0.245, for the more metal-poor composition, up to 0.303 for the more metal-rich one, with ΔY/ΔZ ~ 1.4. For each adopted chemical composition, the evolutionary models have been computed without (canonical models) and with overshooting from the Schwarzschild boundary of the convective cores during the central H-burning phase. Semiconvection is included in the treatment of core convection during the He-burning phase. The whole set of evolutionary models can be used to compute isochrones in a wide age range, from ~30 Myr to ~15 Gyr. Both evolutionary models and isochrones are available in several observational planes, employing an updated set of bolometric corrections and color-Teff relations computed for this project. The number of points along the models and the resulting isochrones is selected in such a way that interpolation for intermediate metallicities not contained in the grid is straightforward; a simple quadratic interpolation produces results of sufficient accuracy for population synthesis applications.We compare our isochrones with results from a series of widely used stellar evolution databases and perform some empirical tests for the reliability of our models. Since this work is devoted to scaled solar chemical compositions, we focus our attention on the Galactic disk stellar populations, employing multicolor photometry of unevolved field main-sequence stars with precise Hipparcos parallaxes, well-studied open clusters, and one eclipsing binary system with precise measurements of masses, radii, and [Fe/H] of both components. We find that the predicted metallicity dependence of the location of the lower, unevolved main sequence in the color magnitude diagram (CMD) appears in satisfactory agreement with empirical data. When comparing our models with CMDs of selected, well-studied, open clusters, once again we were able to properly match the whole observed evolutionary sequences by assuming cluster distance and reddening estimates in satisfactory agreement with empirical evaluations of these quantities. In general, models including overshooting during the H-burning phase provide a better match to the observations, at least for ages below ~4 Gyr. At [Fe/H] around solar and higher ages (i.e., smaller convective cores) before the onset of radiative cores, the selected efficiency of core overshooting may be too high in our model, as well as in various other models in the literature. Since we also provide canonical models, the reader is strongly encouraged to always compare the results from both sets in this critical age range.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/814f4b8a3cd1adeffc9884b1f26582157f7a7b0d

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In Astronomy and Astrophysics

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Citations in the corpus

• On the galaxy stellar mass function, the mass-metallicity relation, and the implied baryonic mass function (2008, background): “BaSTI (M. Salaris, private communication; Pietrinferni et al. 2004).”
• Homogeneous studies of transiting extrasolar planets – IV. Thirty systems with space-based light curves (2011, background): “As in Paper III Iuse five sets of model predictions:Claret (Claret 2004, 2005, 2006, 2007), Y2 (Demarque et al. 2004),Teramo(Pietrinferni et al. 2004),VRSS (VandenBerg et al. 2006) andDSEP(Dotter et al. 2008).”
• THE APOGEE RED-CLUMP CATALOG: PRECISE DISTANCES, VELOCITIES, AND HIGH-RESOLUTION ELEMENTAL ABUNDANCES OVER A LARGE AREA OF THE MILKY WAY'S DISK (2014, methodology): “We have also computed the density near the RC using the Padova (Girardi et al. 2000; Bonatto et al. 2004) and BaSTI (Pietrinferni et al. 2004) isochrone libraries using the same IMF and SFH assumptions.”
• THE METALLICITY DISTRIBUTION FUNCTIONS OF SEGUE G AND K DWARFS: CONSTRAINTS FOR DISK CHEMICAL EVOLUTION AND FORMATION (2011, methodology): “Finally, these models are built using the BaSTI isochrones (Pietrinferni et al. 2004), which they artificially widen to simulate the photometric errors of SDSS.”
• The structure of the Milky Way's bar outside the bulge (2015, methodology): “The luminosity function ΦµK is calculated from the BASTI isochrones (Pietrinferni et al. 2004).”
• The Multiplicity of the Subgiant Branch of ω Centauri: Evidence for Prolonged Star Formation (2007, methodology): “The relation between color and TeA, as a function of [M/H] (by which we mean the global metallicity, including -enhancement), was derived from isochrones by Pietrinferni et al. (2004, 2006).”
• A Large Stellar Evolution Database for Population Synthesis Studies. II. Stellar Models and Isochrones for an α-enhanced Metal Distribution (2006, background): “We have recently published (Pietrinferni et al. 2004, hereafter Paper I) an extended database of scaled-solar stellar evolution models and isochrones that is very well suited to accomplish this goal.”
• FUNDAMENTAL PROPERTIES OF KEPLER PLANET-CANDIDATE HOST STARS USING ASTEROSEISMOLOGY (2013, neutral): “…we have used different model tracks: the Aarhus Stellar Evolution Code (ASTEC; Christensen-Dalsgaard 2008), the Bag of STellar Isochrones (BaSTI; Pietrinferni et al. 2004), the Dartmouth Stellar Evolution Database (DSEP; Dotter et al. 2008), the Padova stellar evolution code (Marigo et al.…”
• Mapping the three-dimensional density of the galactic bulge with VVV red clump stars (2013, methodology): “We simulate stars drawn from the metallicity distribution function (MDF) in the direction of Baade’s window measured by Zoccali et al. (2008), with age 10Gyr, and draw masses from an initial mass function (IMF).”
• 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).”
• Near-Infrared Properties of 24 Globular Clusters in the Galactic Bulge (2006, neutral): “…metallicity, together with the new best-fit relations: M bump Bol ¼ 1:93þ 1:73½Fe=H þ 0:29½Fe=H 2; ð7Þ M bump Bol ¼ 1:62þ 1:61½M=H þ 0:28½M=H 2: ð8Þ The comparison between the data and the theoretical models by Straniero et al. (1997), Girardi et al. (2000), and Pietrinferni et al. (2004) (see Fig.”
• Metallicities on the Double Main Sequence of ω Centauri Imply Large Helium Enhancement (2004, methodology): “Unlike Pietrinferni et al. (2004), however, in the present work we assumed [α/Fe] = 0.4; the alpha-enhanced models will be published in a forthcoming paper.”
• MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS (2016, methodology): “The former is likely mostly due to differences in the adopted boundary conditions in the models, and the latter is possibly due to differences in the adopted Reimers mass loss efficiency (BaSTI, PARSEC, and MIST adopt ηR = 0.4, 0.2, and 0.1, respectively, while Y2 does not include mass loss).”
• FUNDAMENTAL PROPERTIES OF STARS USING ASTEROSEISMOLOGY FROM KEPLER AND CoRoT AND INTERFEROMETRY FROM THE CHARA ARRAY (2012, methodology): “We use the publicly available BaSTI stellar evolutionary tracks (Pietrinferni et al. 2004) with solar-scaled distribution of heavy elements (Grevesse & Noels 1993) and a standard mass loss parameter of η = 0.4 (see, e.g. Fusi-Pecci & Renzini 1976).”
• Scaled solar tracks and isochrones in a large region of the Z-Y plane. II. From 2.5 to 20 solar masses (2009, methodology): “Bono et al. (2000) presented intermediate-mass standard models with different helium and metal content (3≤ M ≤ 15M⊙), and Pietrinferni et al. (2004, 2006) database makes available stellar models and isochrones for scaled-solar andα-enhanced metal distributions in the mass range between 0.5 and 10M⊙…”
• Homogeneous studies of transiting extrasolar planets - III. Additional planets and stellar models (2010, methodology): “The third model set used here isTeramo8 (Pietrinferni et al. 2004), and I selected the ones with moderate convective core overshooting (for masses >1.1M⊙), the standard mass loss law (η = 0.4) and normal elemental abundances (scaled-solar, i.e. no enhancement of the αelements).”
• Evolution of Stars and Stellar Populations (2005, background): “1 HRD of selected stellar evolutionary tracks (dashed lines) with the same initial solar chemical composition and the labelled masses (from [152]).”
• Ages and fundamental properties of Kepler exoplanet host stars from asteroseismology (2015, methodology): “A linear fit to the initial abundances of a solar calibration results in a relation close to ∆Y/∆Z = 1.4, which is the one adopted in our grids (see e.g., Pietrinferni et al. 2004).”
• Gaia broad band photometry (2010, methodology): “Recently, new stellar evolution models appeared in the Padova database for low-mass stars and high-mass stars in a large region of the 15M⊙) and the Pietrinferni et al. (2004, 2006) extended database makes available stellar models and isochrones for scaled-solar andα-enhanced metal distribution for…”
• AGE DETERMINATION OF SIX INTERMEDIATE-AGE SMALL MAGELLANIC CLOUD STAR CLUSTERS WITH HST/ACS (2008, neutral): “We fitted our m555 vs m555-m814 CMDs with three different isochrone models: Padova isochrones (L. Girardi 2006, private communication, Girardi et al. 2000)10, Teramo isochrones (Pietrinferni et al. 2004) and Dartmouth isochrones (Dotter et al. 2007), all with scaled solar abundances ([α/Fe]=0.0).”