On Ultraviolet Fluxes, Bolometric Corrections and Effective Temperatures of Late B to F Stars

Observed ultraviolet fluxes have been compared with the predictions of line blanketed model atmospheres for stars of spectral type later than B5. The comparison reveals significant differences which increase towards later spectral type and which lead to differences between empirical and theoretical bolometric corrections. Empirical bolometric corrections for the spectral range B8–F5 have been computed from a combination of ultraviolet, visual and infrared observational data. These have been used to derive empirically based effective temperatures for five A and F type stars for which angular diameter measurements are available.