On the effective temperature scale of O stars

Details On the effective temperature scale of O stars On the effective temperature scale of O stars

2001-11-13

arxiv.org/abs/astro-ph/0111233v1

Astron.Astrophys.382:999-1004,2002

Astronomy and Astrophysics

Astrophysics

6 pages, 4 figures. To be published in A&A

Scientific paper

10.1051/0004-6361:20011703

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.

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