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Quantitative Analysis of O-Type Stars Properties, at Low Metallicity

Published online by Cambridge University Press:  26 May 2016

Jean-Claude Bouret ,
Thierry M. Lanz ,
Sara R. Heap ,
Ivan Hubeny ,
D. John Hillier ,
Daniel J. Lennon ,
Christopher J. Evans  and
Linda J. Smith
Jean-Claude Bouret
Affiliation:
Laboratoire d'Astrophysique de Marseille, Traverse du Siphon - BP 8, F-13376 Marseille Cedex 12, la France
Thierry M. Lanz
Affiliation:
Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, Code 681, Greenbelt, MD 20771, USA
Sara R. Heap
Affiliation:
Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, Code 681, Greenbelt, MD 20771, USA
Ivan Hubeny
Affiliation:
Laboratory for Astronomy and Solar Physics, NASA Goddard Space Flight Center, Code 681, Greenbelt, MD 20771, USA
D. John Hillier
Affiliation:
Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260, USA
Daniel J. Lennon
Affiliation:
Isaac Newton Group of Telescopes, E-38700 Santa Cruz de La Palma, Canary Islands, España
Christopher J. Evans
Affiliation:
Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK
Linda J. Smith
Affiliation:
Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, UK

Abstract

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We have investigated the properties of main-sequence O-type stars in the SMC. Mass-loss rates, luminosities and Teff are much smaller for these stars than for Galactic ones, resulting in a steeper wind-momentum relation.

Type
Part 1. Atmospheres of Massive Stars
Information
Symposium - International Astronomical Union , Volume 212: A Massive Star Odyssey: From Main Sequence to Supernova , 2003 , pp. 156 - 157
Copyright
Copyright © Astronomical Society of the Pacific 2003 

References

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