The Pisa pre-main sequence tracks and isochrones - A database covering a wide range of Z, Y, mass, and age values

By E. Tognelli, P. Moroni, S. Degl'innocenti. 2011

227 citations recorded by the source corpus.

Context. In recent years new observations of pre-main sequence stars (pre-MS) with Z≤ Z⊙ have been made available. To take full advantage of the continuously growing amount of data of pre-MS stars in different environments, we need to develop updated pre-MS models for a wide range of metallicity to assign reliable ages and masses to the observed stars. Aims. We present updated evolutionary pre-MS models and isochrones for a fine grid of mass, age, metallicity, and helium values . Methods. We use a standard and well-tested stellar evolutionary code (i.e. FRANEC), that adopts outer boundary conditions from detailed and realistic atmosphere models. In this code, we incorporate additional improvements to the physical inputs related to the equation of state and the low temperature radiative opacities essential to computing low-mass stellar models. Results. We make available via internet a large database of pre-MS tracks and isochrones for a wide range of chemical compositions (Z = 0.0002− 0.03), masses (M = 0.2− 7.0 M⊙), and ages (1− 100 Myr) for a solar-calibrated mixing length parameterα (i.e. 1.68). For each chemical composition, additional models were computed with two different mixing length values, namelyα = 1.2 and 1.9. Moreover, for Z≥ 0.008, we also provided models with two different initial deuterium abundances. The characteristics o f the models have been discussed in detail and compared with other work in the literature. The main uncertainties affecting theoretical predictions have been critically discussed. Comparisons with selected data indicate that there is close agreement between theory and observation.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/12a0ab08aa0987254d7f905aeace6f9444bddc62

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In Astronomy and Astrophysics

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Citations in the corpus

• The star formation history and accretion-disc fraction among the K-type members of the Scorpius–Centaurus OB association (2016, methodology): “We use the Dartmouth models (Dotter et al. 2008), the Pisa models (Tognelli et al. 2011), the PARSEC models (Chen et al. 2014), and the Exeter/Lyon models (Baraffe et al. 2015).”
• Mind Your Ps and Qs: The Interrelation between Period (P) and Mass-ratio (Q) Distributions of Binary Stars (2016, methodology): “To determine our own values of q from the brightness contrasts ∆m, we utilize the solar-metallicity pre-MS and MS stellar evolutionary tracks from Tognelli et al. (2011) and Bertelli et al. (2009), respectively.”
• MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS (2016, background): “They found that none of the considered models—Lyon (Baraffe et al. 2015), Dartmouth (Dotter et al. 2008), Pisa (Tognelli et al. 2011), Siess (Siess et al. 2000), and PARSEC (Chen et al. 2014)—predicted an age around ∼ 11 Myr given the system’s stellar properties.23 A simple exercise where they…”
• BANYAN. XI. The BANYAN Σ Multivariate Bayesian Algorithm to Identify Members of Young Associations with 150 pc (2018, background): “Gennaro et al. (2012) estimated the age of the eclipsing binary system TY CrA between 3.8+2.7−0.2 Myr and 5.2+3.1−0.7 Myr, based on a comparison of the dynamical masses of its components with a set of warm and cold PISA pre-main sequence models (Tognelli et al. 2011), respectively.”
• A self-consistent, absolute isochronal age scale for young moving groups in the solar neighbourhood (2015, methodology): “In this study we adopt four sets of semi-empirical model isochrones based on different interior models, namely the Dotter et al. (2008), Tognelli et al. (2011), Bressan et al. (2012) and Baraffe et al. (2015) models (hereafter referred to as Dartmouth, Pisa, PARSEC and BHAC15 respectively)1.”
• Volatile carbon locking and release in protoplanetary disks. A study of TW Hya and HD 100546 (2016, background): “Blackbody spectra of pre main sequence model stars from Tognelli et al. (2011) for an age of 10 Myr are provided for comparison.”
• Discovery of a planetary-mass companion within the gap of the transition disk around PDS 70 (2018, methodology): “We compare the position of PDS 70 with the PMS evolutionary tracks and isochrones from Tognelli et al. (2011) in Fig.”
• MESA ISOCHRONES AND STELLAR TRACKS (MIST) 0: METHODS FOR THE CONSTRUCTION OF STELLAR ISOCHRONES (2016, methodology): “…the isochrone libraries in use today, such as BaSTI (Pietrinferni et al. 2004), Dartmouth (Dotter et al. 2008), PARSEC (Bressan et al. 2012), Pisa (Tognelli et al. 2011), Victoria-Regina (VandenBerg et al. 2006), and YaleYonsei (Yi et al. 2001), are based on the more-sophisticated approach, one…”
• AN OPTICAL SPECTROSCOPIC STUDY OF T TAURI STARS. I. PHOTOSPHERIC PROPERTIES (2014, methodology): “The pre-main sequence tracks applied here to calculate masses and ages are combined from Tognelli et al. (2011) and Baraffe et al. (2003), as described in Appendix C. 4.3.1.”
• The Updated BaSTI Stellar Evolution Models and Isochrones. I. Solar-scaled Calculations (2018, methodology): “For the comparison we have selected Tognelli et al. (2011) calculations (that at fixed Z allow for various choices of Y , the deuterium mass fraction XD and mixing length) for Z=0.0175, Y=0.265 XD = 4 10 −5, αML=1.9 –very close to our initial solar chemical composition, the adopted initial…”