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Quantitative spectroscopy of OB stars: from dwarfs to supergiants

Published online by Cambridge University Press:  25 February 2014

N. Przybilla ,
M.F. Nieva ,
M. Firnstein  and
K. Butler
N. Przybilla
Affiliation:
Institute for Astro- and Particle Physics, University of Innsbruck, Technikerstr. 25/8, 6020 Innsbruck, Austria
M.F. Nieva
Affiliation:
Institute for Astro- and Particle Physics, University of Innsbruck, Technikerstr. 25/8, 6020 Innsbruck, Austria Dr. Karl Remeis-Observatory & ECAP, University of Erlangen-Nuremberg, Sternwartstr. 7, 96049 Bamberg, Germany
M. Firnstein
Affiliation:
Dr. Karl Remeis-Observatory & ECAP, University of Erlangen-Nuremberg, Sternwartstr. 7, 96049 Bamberg, Germany
K. Butler
Affiliation:
University Observatory, University of Munich, Scheinerstr. 1, 81679 Munich, Germany
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Abstract

We discuss recent progress made in the spectral modelling of OB stars from the main sequence to evolved phases as BA-type supergiants. Non-LTE line-formation computations can now reproduce observed spectra over the entire optical and near-IR wavelength range with high confidence, facilitating stellar atmospheric parameters and elemental abundances to be determined at high accuracy and precision. An overview is given how the fundamental stellar parameters of single stars determined in our new approach compare to high-precision data derived from detached eclipsing massive binary stars. Finally, the observational constraints for a sample of Galactic objects are put in context with state-of-the-art evolution models for rotating massive stars.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 64: Setting a New Standard in the Analysis of Binary Stars , 2013 , pp. 37 - 45
Copyright
© EAS, EDP Sciences, 2014

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