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HD 152246, a new high-mass triple system – preliminary results

Published online by Cambridge University Press:  25 February 2014

A. Nasseri ,
R. Chini ,
P. Harmanec ,
P. Mayer ,
T. Dembsky ,
H. Lehmann  and
H. Sana
A. Nasseri
Affiliation:
Astronomisches Institut, Ruhr-Universität Bochum, Germany,
R. Chini
Affiliation:
Astronomisches Institut, Ruhr-Universität Bochum, Germany, Instituto de Astronomía, Universidad Católica del Norte, Antofagasta, Chile
P. Harmanec
Affiliation:
Astronomical Institute of the Charles University, Faculty of Mathematics and Physics, Praha, Czech Republic
P. Mayer
Affiliation:
Astronomical Institute of the Charles University, Faculty of Mathematics and Physics, Praha, Czech Republic
T. Dembsky
Affiliation:
Astronomisches Institut, Ruhr-Universität Bochum, Germany,
H. Lehmann
Affiliation:
Thüringer Landessternwarte Tautenburg, Germany
H. Sana
Affiliation:
Space Telescope Science Institute, Baltimore, USA
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Abstract

Multi-epoch, high-resolution (R ∼ 50 000) optical spectrosco-py of the O-type (O9 III – IV) star HD 152246 suggests that it is a triple system where a close inner pair (Aa–Ab) with a circular orbit and a period of 6 days is in a 53–d eccentric orbit (e = 0.68) with a third component Ac. The mass ratios for the inner and outer system are 0.10 and 0.96, respectively. The strengths of various He lines classify Aa and Ac as late O-type stars while Ab is invisible in our spectra.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 64: Setting a New Standard in the Analysis of Binary Stars , 2013 , pp. 411 - 412
Copyright
© EAS, EDP Sciences, 2014

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References

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Sana, H., Gosset, E., Rauw, G., et al, 2006, A&A, 454, 1047
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