  We rediscuss the temperature of O dwarfs based on new non-LTE line blanketed
atmosphere models including stellar winds computed with the CMFGEN code of
Hillier & Miller (1998). Compared to the latest calibration of Vacca et al.
(1996), the inclusion of line blanketing leads to lower effective temperatures,
typically by 4000 to 1500 K for O3 to O9.5 dwarf stars. The dependence of the
Teff-scale on stellar and model parameters - such as mass loss,
microturbulence, and metallicity - is explored, and model predictions are
compared to optical observations of O stars. Even for an SMC metallicity we
find a non-negligible effect of line blanketing on the Teff-scale. The
temperature reduction implies downward revisions of luminosities by 0.1 dex and
Lyman continuum fluxes Q0 by approximately 40% for dwarfs of a given spectral
type.
