The Physical Properties and Effective Temperature Scale of O-type Stars as a Function of Metallicity. II. Analysis of 20 More Magellanic Cloud Stars, and Results from the Complete Sample

Details The Physical Properties and Effective Temperature Scale of O-type Stars as a Function of Metallicity. II. Analysis of 20 More Magellanic Cloud Stars, and Results from the Complete Sample The Physical Properties and Effective Temperature Scale of O-type Stars as a Function of Metallicity. II. Analysis of 20 More Magellanic Cloud Stars, and Results from the Complete Sample

2005-03-22

arxiv.org/abs/astro-ph/0503464v2

Astrophys.J. 627 (2005) 477-519

Astronomy and Astrophysics

Astrophysics

Accepted by the Astrophysical Journal. A version with higher-resolution figures may be found at ftp://ftp.lowell.edu/pub/mas

Scientific paper

10.1086/430417

We analyze the optical and UV spectra of an additional sample of 20 Magellanic Cloud O stars, and draw conclusions from the complete sample of 40 stars. We find (1) The SMC O3-7 dwarfs are about 4000 K cooler than their Galactic counterparts; this is in the sense expected from the decreased signficiance of line-blanketing and wind-blanketing at lower metallicities. The difference decreases with later types, becoming negligible by B0 V. A similar difference is found for the supergiants. (2) The wind momentum of these stars scales with luminosity and metallicty in the ways predicted by radiatively-driven wind theory. (3) A comparison of the masses derived from spectroscopy with those derived from stellar evolutionary theory shows a significant discrepancy for stars hotter than 45000, although good agreement is found for cooler stars. (4) For the hottest O stars (O2-3.5) neither the NIII/NIV ratio, nor even the HeI/HeII ratio, does a good job of predicting the effective temperature by itself. Instead, a full analysis is needed to derive physical parameters. Thus there are O3.5V stars which are as hot or hotter than stars classified as O2V. (5) The two stars with the most discordant radial velocities in our sample happen to be O3 "field stars". This provides the first compelling observational evidence that the "field" O stars in the Magellanic Clouds may be runaway OB stars, ejected from their birth place.

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