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A critical comparison of spectroscopic and evolutionary masses for O-type binary systems

Published online by Cambridge University Press:  26 May 2016

Laura R. Penny ,
Douglas R. Gies ,
William G. Bagnuolo ,
John H. Wise ,
Artemio Herrero ,
David J. Stickland  and
Chris Lloyd
Laura R. Penny
Affiliation:
Department of Physics and Astronomy, College of Charleston, Charleston, SC 29424, USA
Douglas R. Gies
Affiliation:
Center for High Angular Resolution Astronomy, Department of Physics and Astronomy, Georgia State University, Atlanta, GA 30303, USA
William G. Bagnuolo
Affiliation:
Center for High Angular Resolution Astronomy, Department of Physics and Astronomy, Georgia State University, Atlanta, GA 30303, USA
John H. Wise
Affiliation:
Center for High Angular Resolution Astronomy, Department of Physics and Astronomy, Georgia State University, Atlanta, GA 30303, USA
Artemio Herrero
Affiliation:
Instituto de Astrofísica de Canarias, C/ Vía Láctea s/n, E-38200 La Laguna, Tenerife, Spain
David J. Stickland
Affiliation:
Rutherford Appleton Laboratory, Chilton, Didcot, Oxon OX11 0QX, UK
Chris Lloyd
Affiliation:
Rutherford Appleton Laboratory, Chilton, Didcot, Oxon OX11 0QX, UK

Abstract

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We have embarked on a program to directly compare spectroscopic and evolutionary masses with those obtained from a combination of spectroscopic and photometric orbital solutions for O-type binary systems. The ability to directly determine the spectroscopic masses of the individual components of O-type binary systems has been difficult, because of the severe line blending that is present in these systems. Doppler tomography is an iterative scheme, that uses an ensemble of spectra to reconstruct the individual component spectra. These individual spectra can then be analyzed.

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. 216 - 217
Copyright
Copyright © Astronomical Society of the Pacific 2003 

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