Atmospheric parameters in metal-poor stars. I (Gratton+, 1996)

Details Atmospheric parameters in metal-poor stars. I (Gratton+, 1996) Atmospheric parameters in metal-poor stars. I (Gratton+, 1996)

Oct 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996ycat..33140191g&link_type=abstract

VizieR On-line Data Catalog: J/A+A/314/191. Originally published in: 1996A&A...314..191G

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Stars: Metal-Deficient, Abundances

Scientific paper

We present atmospheric parameters for about 300 stars of different chemical composition, whose spectra will be used to study the galactic enrichment of Fe and light elements. These parameters were derived using an homogeneous iterative procedure, which considers new calibrations of colour-Teff relations for F, G and K-type stars based on Infrared Flux Method (IRFM) and interferometric diameters for population I stars, and the Kurucz (1992) model atmospheres. We found that these calibrations yield a self-consistent set of atmospheric parameters for Teff>4400K, representing a clear improvement over results obtained with older model atmospheres. Using this Teff -scale and Fe equilibrium of ionization, we obtained very low gravities (implying luminosities incompatible with that expected for RGB stars) for metal-poor stars cooler than 4400K; this might be due either to a moderate Fe overionization (expected from statistical equilibrium calculations) or to inadequacy of Kurucz models to describe the atmospheres of very cool giants. Our Teff scale is compared with other scales recently used for metal-poor stars; it agrees well with those obtained using Kurucz (1992) models, but it gives much larger Teff's than those obtained using OSMARCS models (Edvardsson et al. 1993). This difference is attributed to the different treatment of convection in the two sets of models. For the Sun, the Kurucz (1992) model appears to be preferable to the OSMARCS ones because it better predicts the solar limb darkening; furthermore, we find that our photometric Teff 's for metal-poor stars agree well with both direct estimates based on the IRFM, and with Teff's derived from Hα wings when using Kurucz models. (1 data file).

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