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Stellar multiplicity across the mass spectrum

Published online by Cambridge University Press:  25 February 2014

R. Chini ,
A. Nasseri ,
T. Dembsky ,
L.-S. Buda ,
K. Fuhrmann  and
H. Lehmann
R. Chini
Affiliation:
Astronomisches Institut, Ruhr-Universität Bochum, Germany Instituto de Astronomía, Universidad Católica del Norte, Antofagasta, Chile
A. Nasseri
Affiliation:
Astronomisches Institut, Ruhr-Universität Bochum, Germany
T. Dembsky
Affiliation:
Astronomisches Institut, Ruhr-Universität Bochum, Germany
L.-S. Buda
Affiliation:
Astronomisches Institut, Ruhr-Universität Bochum, Germany
K. Fuhrmann
Affiliation:
Astronomisches Institut, Ruhr-Universität Bochum, Germany
H. Lehmann
Affiliation:
Thüringer Landessternwarte Tautenburg, Germany
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Abstract

We investigate the multiplicity as a function of stellar mass. For this purpose we have created three complete samples of O, B, and FGK stars and performed multi-epoch, high-resolution (R ∼ 50 000) optical spectroscopy. The current results for the O-type stars suggest a multiplicity fraction of more than 80%. Many O-type systems contain components of similar mass. The multiplicity fraction for B stars seems to decrease from 70% to 20%. We argue that this general decrease is most likely due to observational biases; however, similar-mass systems – like common for O-type stars – seem to vanish toward later B-types. Within the sample of F stars we observe an increasing multiplicity fraction with primary mass (∼50% – 80%); simultaneously there is a decrease of single stars toward the A-type regime. Closer inspection of spectroscopic binaries – either by spectral disentangling or by common proper motion studies – reveals higher-level systems in each mass range.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 64: Setting a New Standard in the Analysis of Binary Stars , 2013 , pp. 155 - 162
Copyright
© EAS, EDP Sciences, 2014

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