The Y2 Stellar Evolutionary Tracks

By S. Yi, Yong-Cheol Kim, P. Demarque. 2002

243 citations recorded by the source corpus.

We present a database of the latest stellar models of the Y2 (Yonsei-Yale) collaboration. This database contains the stellar evolutionary tracks from the pre-main-sequence birthline to the helium core flash that were used to construct the Y2 isochrones. We also provide a simple interpolation routine that generates stellar tracks for given sets of parameters (metallicity, mass, and α-enhancement).

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/decd91fc4ece7e08a0b9ac43d3bd1efdeaef17a1

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Citations in the corpus

The ACS Survey of Galactic Globular Clusters. II. Stellar Evolution Tracks, Isochrones, Luminosity Functions, and Synthetic Horizontal-Branch Models (2007, background): “…Vandenberg et al. (2006, hereafter Victoria-Regina), Girardi et al. (2002); Bonatto et al. (2004); Girardi et al. (2004, hereafter Padova), Pietrinferni et al. (2004, 2006, hereafter BaSTI) and Cordier et al. (2007), and Yi et al. (2003, 2004); Demarque et al. (2004, hereafter Y2 (Yonsei-Yale)).”
OXYGEN ABUNDANCES IN NEARBY FGK STARS AND THE GALACTIC CHEMICAL EVOLUTION OF THE LOCAL DISK AND HALO (2013, methodology): “We used the Yonsei-Yale isochrones, which take into account α-element enhancement at low metallicities (Yi et al. 2001, 2003; Kim et al. 2002).”
alpha-, r-, and s-process element trends in the Galactic thin and thick disks (2004, background): “In summary the main ingredients are: Effective temperature (Teff) is determined by requiring Fe lines with different lower excitation potentials to give equal abundances; Stellar mass (M) is estimated from the evolutionary tracks by Yi et al. (2003).”
High-precision abundances of elements in solar twin stars - Trends with stellar age and elemental condensation temperature (2015, methodology): “Stellar masses were obtained by interpolating in the luminosity - logTeff diagram between the Yonsei -Yale evolutionary tracks of Yi et al. (2003); see Nissen & Schuster (2012) for details.”
STELLAR DIAMETERS AND TEMPERATURES. III. MAIN-SEQUENCE A, F, G, AND K STARS: ADDITIONAL HIGH-PRECISION MEASUREMENTS AND EMPIRICAL RELATIONS (2013, methodology): “We derive ages and masses for stars in Table 3 by fitting the measured radii and temperatures to the Yonsei-Yale (Y 2) stellar isochrones (Demarque et al. 2004; Yi et al. 2003; Kim et al. 2002; Yi et al. 2001).”
Evolutionary population synthesis: models, analysis of the ingredients and application to high‐z galaxies (2004, background): “The temperatures of the RGB, especially towards the tip are cooler in the Padova tracks, at solar metallicity and above,a f ature also found in the Yale tracks of Yi et al. (2003).”
Y2 Isochrones with an Improved Core Overshoot Treatment (2004, unknown): “The purpose of this paper is to improve on the treatment of convective core overshoot in the Y 2 isochrones (Yi et al. 2001, hereafter Paper I; Kim et al. 2002, hereafter Paper II; Yi et al. 2003).”
Decay of Planetary Debris Disks (2005, methodology): “To convert the H-R diagram placements to stellar age, we used the Y2 isochrones from Yi et al. (2003).”
A Robust Measure of Tidal Circularization in Coeval Binary Populations: The Solar-Type Spectroscopic Binary Population in the Open Cluster M35 (2004, methodology): “Masses are derived using the Yale (Y2) stellar evolution models (Yi et al. 2003).”
STELLAR ROTATION IN M35: MASS–PERIOD RELATIONS, SPIN-DOWN RATES, AND GYROCHRONOLOGY (2008, methodology): “The color indices derive from the deep multi-band photometry by Deliyannis (2008, Section 2.5) and the corresponding stellar mass estimates (upper x-axis) from a fit of a 150Myr Yale stellar evolutionary model (Yi et al. 2003) to the M35 color-magnitude diagram.”
A Spectroscopic Study of the Ancient Milky Way: F- and G-Type Stars in the Third Data Release of the Sloan Digital Sky Survey (2005, methodology): “We note that the predicted surface temperatures for turnoff stars in the Yonsei-Yale isochrones (Yi et al. 2003) are very similar to those used here.”