The empirical BC versus T EFF scale for non-supergiant O9-G5 stars.

Abstract

By the analysis of observed energy distributions extending from the UV to the IR, the effective temperature, the gravity and the bolometric correction for a representative sample of nonsupergiant and not chemically peculiar O9-G5 stars are derived in a self-consistent way. The new, improved relationship between the bolometric correction and the effective temperature is then compared to the theoretical or observed ones previously published. The method used permits the derivation of angular diameters for the stars, with an uncertainty on the same order as the errors quoted for interferometric measurements. The importance of these results in the calibration of stellar parameters is stressed and their relevance for a direct comparison between the theoretical and the observational HR diagrams is briefly mentioned.