Astrophys. J., 794, 72 (2014/October-2)
Isochrones for old (>5 gyr) stars and stellar populations. I. Models for -2.4 ≤ [Fe/H] ≤ +0.6, 0.25 ≤ y ≤ 0.33, and -0.4 ≤ [α/Fe] ≤ +0.4.
VANDENBERG D.A., BERGBUSCH P.A., FERGUSON J.W. and EDVARDSSON B.
Abstract (from CDS):
Canonical grids of stellar evolutionary sequences have been computed for the helium mass-fraction abundances Y = 0.25, 0.29, and 0.33, and for iron abundances that vary from -2.4 to +0.4 (in 0.2 dex increments) when [α/Fe] =+0.4, or for the ranges -2.0 ≤ [Fe/H] ≤ +0.6, -1.8 ≤ [Fe/H] ≤ +0.6 when [α/Fe] =0.0 and -0.4, respectively. The grids, which consist of tracks for masses from 0.12M☉ to 1.1-1.5M☉ (depending on the metallicity) are based on up-to-date physics, including the gravitational settling of helium (but not metals diffusion). Interpolation software is provided to generate isochrones for arbitrary ages between ~5 and 15 Gyr and any values of Y, [α/Fe], and [Fe/H] within the aformentioned ranges. Comparisons of isochrones with published color-magnitude diagrams (CMDs) for the open clusters M67 ([Fe/H] ~0.0) and NGC 6791 ([Fe/H] ~0.3) and for four of the metal-poor globular clusters (47 Tuc, M3, M5, and M92) indicate that the models for the observed metallicities do a reasonably good job of reproducing the locations and slopes of the cluster main sequences and giant branches. The same conclusion is reached from a consideration of plots of nearby subdwarfs that have accurate Hipparcos parallaxes and metallicities in the range -2.0 ≲ [Fe/H] ≲ -1.0 on various CMDs and on the (log Teff, MV) diagram. A relatively hot temperature scale similar to that derived in recent calibrations of the infrared flux method is favored by both the isochrones and the adopted color transformations, which are based on the latest MARCS model atmospheres.
globular clusters: individual: (47 Tuc, M3, M5, M92) - open clusters and associations: individual: (M67, NGC 6791) - stars: abundances - stars: evolution - stars: Population II
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