parsec: stellar tracks and isochrones with the PAdova and TRieste Stellar Evolution Code

By A. Bressan, P. Marigo, L. Girardi, B. Salasnich, Claudia Dal Cero, S. Rubele, A. Nanni. 2012

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We present the updated version of the code used to compute stellar evolutionary tracks in Padova. It is the result of a thorough revision of the major in put physics, together with the inclusion of the pre‐main sequence phase, not present in our previous releases of stellar models. Another innovative aspect is the possibility of prompt ly generating accurate opacity tables fully consistent with any selected initial chemical composition, by coupling the OPAL opacity data at high temperatures to the molecular opacities computed with our AESOPUS code (Marigo & Aringer 2009). In this work we present extended sets of stellar evolutionary models for various initial chemical compositions, while other set s with different metallicities and/or different distributions of heavy elements are being computed. For the present release of models we adopt the solar distribution of heavy elements from the recent revision by Caffau et al. (2011), corresponding to a Sun’s metallicity Z≃ 0.0152. From all computed sets of stellar tracks, we also derive isochrones in several photometric systems. The aim is to provide the community with the basic tools to model star clusters and galaxies by means of population synthesis techniques.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/d1dd4db23461673dbe3ac36dee6087b78c751f2a

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Citations in the corpus

New PARSEC evolutionary tracks of massive stars at low metallicity: testing canonical stellar evolution in nearby star-forming dwarf galaxies (2014, methodology): “Since our stellar evolution code has been deeply revised recently (Girardi et al. 2000; Bressan et al. 2012, 2013), we present here new sets of evolutionary tracks of massive stars computed with the PARSEC code.”
The cosmic merger rate of stellar black hole binaries from the Illustris simulation (2017, methodology): “With this relatively small change, we obtain a mass spectrum of BHs similar to the one published by Spera et al. (2015) and based on the MNRAS 000, 000–000 (0000) PARSEC stellar evolution tracks (Bressan et al. 2012; Tang et al. 2014; Chen et al. 2015).”
The White Dwarf Initial–Final Mass Relation for Progenitor Stars from 0.85 to 7.5 M⊙ (2018, methodology): “…based on different stellar evolutionary models, the Yale-Yonsei isochrones (Yi et al. 2001; hereafter Y2 isochrones) and the PARSEC isochrones (Bressan et al. 2012) version 1.2S.7 The ages of each young cluster these white dwarfs are members of were measured with both model isochrones, but…”
A detached stellar-mass black hole candidate in the globular cluster NGC 3201 (2018, methodology): “In order to derive the mass and surface gravity log g for the spectrum fit (see Table 2) of the target star, we compare its HST ACS colour and magnitude with a PARSEC isochrone (Bressan et al. 2012).”
Massive black hole binaries from runaway collisions: the impact of metallicity (2016, methodology): “To avoid unphysical results, we request that the values of the radius of single stars are consistent with PARSEC stellar evolution tracks (Bressan et al. 2012; Tang et al. 2014; Chen et al. 2015) for stars with mass> 100 M⊙, as implemented in our new population synthesis code SEVN (Spera et al.…”
Nuclear activity versus star formation: emission-line diagnostics at ultraviolet and optical wavelengths (2015, methodology): “The presentage solar metallicity adopted in G15 and in this work is Z = 0.01524 (Bressan et al. 2012).”
A Guide to Realistic Uncertainties on the Fundamental Properties of Solar-type Exoplanet Host Stars (2020, neutral): “Numerous model grids are publicly available to allow this (e.g. MIST, Choi et al. 2016, PARSEC, Bressan et al. 2012, DSEP, Dotter et al. 2008, Yonsai—Yale, Spada et al. 2013, etc.) and a variety of tools have been developed to simplify the inference such as isochrones (Morton 2015), isoclassify…”
Stellar Population Inference with Prospector (2020, methodology): “Isochrone libraries are available from the MIST (Choi et al. 2016), PARSEC (Bressan et al. 2012), BaSTI (Cordier et al. 2007), Padova (Marigo et al. 2008), Geneva (Meynet et al. 1994), and BPASS (Eldridge et al. 2017) models.”
Modelling and interpreting spectral energy distributions of galaxies with BEAGLE (2016, methodology): “This version of the code incorporates updated stellar evolutionary tracks (Bressan et al. 2012; Marigo et al. 2013) and the MILES library of observed optical stellar spectra (Sánchez-Blázquez et al. 2006) to describe the properties of stars in the Hertzsprung–Russell diagram [ λ(Lbol, Teff, Z )…”
Modelling the nebular emission from primeval to present-day star-forming galaxies (2016, methodology): “…is that these do not incorporate important advances achieved 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…”
Do Kepler Superflare Stars Really Include Slowly Rotating Sun-like Stars?—Results Using APO 3.5 m Telescope Spectroscopic Observations and Gaia-DR2 Data (2019, methodology): “…estimated stellar radius (Rspec) values from the stellar atmospheric parameters (Teff, log g, and [Fe/H]), by applying the latest PARSEC isochrones (Bressan et al. 2012; Marigo et al. 2017).29 In this process, we used basically the same method as the one used in our previous study (Notsu et al.…”
Very massive stars, pair-instability supernovae and intermediate-mass black holes with the sevn code (2017, methodology): “The default version of SEVN includes a set of input tables generated using the PARSEC code (Bressan et al. 2012; Tang et al. 2014; Chen et al. 2015).”
Chemodynamics of the Milky Way - I. The first year of APOGEE data (2013, methodology): “We have used the newly computed PARSEC isochrones (Bressan et al. 2012), which have a much more detailed grid of theoretical isochrones for the 2MASS JHKs photometric system than the ones previously available.”
The mass spectrum of compact remnants from the parsec stellar evolution tracks (2015, methodology): “Both the models of SN explosion (e.g. Fryer et al. 2012; Janka 2012; Burrows 2013; Clausen et al. 2015; Ertl et al. 2015; Pejcha & Prieto 2015) and the theory of massive star evolution (e.g. Bressan et al. 2012; Tang et al. 2014) were deeply revised in the last few years.”
PARSEC evolutionary tracks of massive stars up to 350 M ☉ at metallicities 0.0001 ≤ Z ≤ 0.04 (2015, methodology): “The input physics used in PARSEC is already thoroughly described in Bressan et al. (2012), Bressan et al. (2013) and Chen et al. (2014).”
Protoplanetary disk lifetimes vs stellar mass and possible implications for giant planet populations (2015, methodology): “These luminosities were transformed into masses using the mass-luminosity relationship given by the pre-main sequence isochrones of the corresponding age in Bressan et al. (2012).”
A catalogue of masses, structural parameters, and velocity dispersion profiles of 112 Milky Way globular clusters (2018, methodology): “We determined the stellar mass functions from the luminosity functions by fitting either Dartmouth (Dotter et al. 2008) or PARSEC isochrones (Bressan et al. 2012) to the HST color-magnitude diagrams.”
GALAXIES AT THE EXTREMES: ULTRA-DIFFUSE GALAXIES IN THE VIRGO CLUSTER (2015, background): “We also overplot 3 the PARSEC isochrones of Bressan et al. (2012) with metallicities Z = 0.00015, Z = 0.0015 and Z = 0.0060 ([M/H]= −2.0, −1.0, and −0.4, respectively).”
Discovery of a warm, dusty giant planet around HIP 65426 (2017, methodology): “neighboring stars Adopting the values from Table A.1, the placement in absolute magnitude in V-band versus effective temperature diagram and comparison with theoretical models by Bressan et al. (2012) yields an age of 9-10 Myr when adopting the Gaia DR1 parallax (Fig.”