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HD 150136: towards one of the most massive systems?

Published online by Cambridge University Press:  12 July 2011

Laurent Mahy ,
Eric Gosset ,
Hugues Sana ,
Gregor Rauw ,
Thomas Fauchez  and
Christian Nitschelm
Laurent Mahy
Affiliation:
Institut d'Astrophysique et de Géophysique, University of Liège, Allée du 6 Août, 17, Bât. B5C, B-4000, Liège, Belgium email: [email protected]
Eric Gosset
Affiliation:
Institut d'Astrophysique et de Géophysique, University of Liège, Allée du 6 Août, 17, Bât. B5C, B-4000, Liège, Belgium email: [email protected]
Hugues Sana
Affiliation:
Sterrenkundig Instituut ‘Anton Pannekoek’, Universiteit van Amsterdam, Postbus 94249, NL-1090 GE Amsterdam, The Netherlands
Gregor Rauw
Affiliation:
Institut d'Astrophysique et de Géophysique, University of Liège, Allée du 6 Août, 17, Bât. B5C, B-4000, Liège, Belgium email: [email protected]
Thomas Fauchez
Affiliation:
Institut d'Astrophysique et de Géophysique, University of Liège, Allée du 6 Août, 17, Bât. B5C, B-4000, Liège, Belgium email: [email protected]
Christian Nitschelm
Affiliation:
Instituto de Astronomía, Universidad Católica del Norte, Avenida Angamos 0610, Antofagasta, Chile
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Abstract

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We present the preliminary results of an intensive monitoring devoted to HD 150136. Already quoted as an O3+O6 binary, we detected a third O-type component physically linked to the system, making it one of the nearest (1.3 kpc) most massive systems known until now (~134M⊙). To determine the physical parameters of this system, we applied a disentangling program to study individually the three components. It allows us to constrain their spectral types and to derive a new orbital solution for the short-period system.

Keywords

stars: individual (HD 150136)binaries: spectroscopicstars: fundamental parameters
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S272: Active OB stars: structure, evolution, mass loss, and critical limits , July 2010 , pp. 521 - 522
Copyright
Copyright © International Astronomical Union 2011

References

González, J. F. & Levato, H. 2006, A&A, 448, 283Google Scholar
Heck, A., Manfroid, J., & Mersch, G. 1985, A&AS, 59, 63Google Scholar
Hillier, D. J. & Miller, D. L. 1998, ApJ, 496, 407CrossRefGoogle Scholar
Mahy, L., Rauw, G., Martins, F., Nazé, Y. et al. 2010, ApJ, 708, 1537ApJ, 708, 1537CrossRefGoogle Scholar
Niemela, V. S. & Gamen, R. C. 2005, MNRAS, 356, 974CrossRefGoogle Scholar
Skinner, S. L., Zhekov, S. A., Palla, F., & Barbosa, C. L. D. R. 2005, MNRAS, 361, 191CrossRefGoogle Scholar