ABUNDANCES OF LIGHT-ELEMENTS IN METAL-POOR STARS .1. ATMOSPHERIC PARAMETERS AND A NEW T-EFF SCALE

We present atmospheric parameters for about 300 stars of different che mical composition, whose spectra will be used to study the galactic en richment of Fe and light elements. These parameters were derived using an homogeneous iterative procedure, which considers new calibrations of colour-T-eff relations for F, G and K-type stars based on Infrared Flux Method (IRFM) and interferometric diameters for population Istars , and the Kurucz(1992) model atmospheres. We found that these calibrat ions yield a self-consistent set of atmospheric parameters for T-eff > 4400 K, representing a clear improvement over results obtained with o lder model atmospheres. Using this T-eff-scale and Fe equilibrium of i onization, we obtained very low gravities (implying luminosities incom patible with that expected for RGB stars) for metal-poor stars cooler than 4400 K; 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 T-eff 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 T-eff's than those obtained using OSMARCS mo dels (Edvardsson et al. 1993). This difference is attributed to the di fferent 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 T-eff's for metal-poor stars agree well with both direct estimates based on the IRFM, and with T-eff's derived fro m H alpha wings when using Kurucz models.