Models for Old, Metal-poor Stars with Enhanced α-Element Abundances. I. Evolutionary Tracks and ZAHB Loci; Observational Constraints

By D. VandenBerg, F. Swenson, F. Rogers, C. Iglesias, D. Alexander. 2000

252 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/de2206d8b4b4a286e4e4043a6f48dc8db849c50b

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

Non‐LTE line formation of Fe in late‐type stars – I. Standard stars with 1D and 〈3D〉 model atmospheres (2012, methodology): “For the other stars, we determined surface gravities from the Hipparcos parallaxes (van Leeuwen 2007) using the masses estimated from the tracks of VandenBerg et al. (2000) by Gehren et al. (2004, 2006) and apparent bolometric magnitudes from Casagrande et al. (2010).”
New constraints on the chemical evolution of the solar neighbourhood and galactic disc(s) - improved astrophysical parameters for the Geneva-Copenhagen Survey (2011, background): “…has been shown that for the range of metallicities covered by the present study, isochrones for enhancedα abundances can be reproduced remarkably well by those for solar scaled mixtures ifZ is the same (e.g., Chieffi et al. 1991; Chaboyer et al. 1992; Salaris & Weiss 1998; VandenBerg et al. 2000).”
The Evolution of the C/O Ratio in Metal-poor Halo Stars (2003, methodology): “The bolometric correction was adopted from the work of Alonso et al. (1995), and the stellar mass was obtained by interpolating in the MV – log Teff diagram between the α-element enhanced evolutionary tracks of VandenBerg et al. (2000).”
The RR Lyrae Period-Luminosity Relation. I. Theoretical Calibration (2004, background): “Note that such a relation should be used with due care for metallicities Z > 0:003 (VandenBerg et al. 2000).”
The Victoria-Regina Stellar Models: Evolutionary Tracks and Isochrones for a Wide Range in Mass and Metallicity that Allow for Empirically Constrained Amounts of Convective Core Overshooting (2005, methodology): “AND ISOCHRONES The code described by VandenBerg et al. (2000) has been used to compute all of the stellar evolutionary sequences that are presented in this investigation.”
Distances and ages of NGC 6397, NGC 6752 and 47 Tuc (2003, background): “…0.57± 0.06 Fourier parameters 0.61± 0.05 Main Sequence Fitting 0.56± 0.07 models (Caloi et al. 1997; Cassisi et al. 1999; Ferraro et al. 1999; Demarque et al. 2000; VandenBerg et al. 2000) agree that although the relation is not universal and not strictly linear, it can be roughly described by a…”
A comparison of stellar populations in galaxy spheroids across a wide range of Hubble types (2002, methodology): “Salaris & Weiss (1998) and VandenBerg et al. (2000) modelled isochrones for the abundance pattern in metal-poor field stars which possess enhancements in α-element abundances as detailed in Section 4.1.”
Updated and Expanded OPAL Equation-of-State Tables: Implications for Helioseismology (2002, methodology): “The noise around logT ¼ 4:7 is apparently due to the stellar model calculation used by SCVH95, since OPAL calculations for the 0.1 M attack from VandenBerg et al. (2000) are smooth.”
NLTE abundances of Mn in a sample of metal-poor stars ⋆ (2008, methodology): “The calculation of the surface gravity acceleration log g is based on hipparcos parallaxes and on masses estimated from tracks of stellar evolution kindly provided by VandenBerg et al. (2000) as indicated in Fuhrmann et al. (1997) or Gehren et al. (2004; 2006).”
An Assessment of Dynamical Mass Constraints on Pre-Main-Sequence Evolutionary Tracks (2003, background): “We assume Mbol; ¼ 4:75 mag in all calculations (Cox 2000; see also footnote 7 in VandenBerg et al. 2000).”
Models for Old, Metal-Poor Stars with Enhanced α-Element Abundances. II. Their Implications for the Ages of the Galaxy’s Globular Clusters and Field Halo Stars (2000, background): “…of the present work is to reexamine all of these issues in the light of a new set of stellar evolutionary computations that is based on up-to-date physics and which treats enhancements in the abundances of the aelements explicitly (see VandenBerg et al. 2000 ; hereafter referred to as Paper I).”
Empirical calibration of the near-infrared Ca II triplet — IV. The stellar population synthesis models (2003, methodology): “For a given total metallicity, the α-enhanced mixtures yield lower opacities, which translates into an increase of the temperature of the stars in the Main Sequence (MS) and the RGB phases (e.g. Salaris & Weiss 1998, hereafter SW98; VandenBerg et al. 2000; Salasnich et al. 2000, hereafter S00; Kim e”
The ACS Survey of Galactic Globular Clusters. II. Stellar Evolution Tracks, Isochrones, Luminosity Functions, and Synthetic Horizontal-Branch Models (2007, background): “…have shown that socalled pseudo-ZAHB (zero age horizontal branch) models that are concocted from red giant branch tip models are nearly indistinguishable from full He flash calculations in terms of the subsequent evolution (Vandenberg et al. 2000; Piersanti et al. 2004; Serenelli & Weiss 2005).”
Population Gradients in Local Group Dwarf Spheroidal Galaxies (2001, background): “For a Ðxed mass, stars with increased [a/Fe] will have lower surface temperatures and therefore will form redder HB stars (VandenBerg et al. 2000 ; VandenBerg & Bell 2001).”
A non-LTE study of neutral and singly-ionized iron line spectra in 1D models of the Sun and selected late-type stars ? (2011, methodology): “To determine log g, we used an updated Hipparcos parallax of πHip = 13.74 ± 0.78 mas from van Leeuwen (2007) and a mass of 0.8 M derived from the tracks of VandenBerg et al. (2000).”
Red Giant Branch Stars: The Theoretical Framework (2002, background): “In particular, as discussed by Salaris, Chieffi & Straniero (1993 – see also Salaris & Cassisi 1996, Salaris & Weiss 1998, Vandenberg et al. 2000), the abundance of low ionization potential elements like Mg, Si, S, Ca and Fe affects strongly the RGB temperature.”
O/Fe in metal-poor main sequence and subgiant stars ? (2002, unknown): “The mass was derived by interpo- lating in the MV – logTeff diagram between the α-element enhanced evolutionary tracks of VandenBerg et al. (2000).”