Hostname: page-component-586b7cd67f-2brh9 Total loading time: 0 Render date: 2024-11-25T22:19:15.189Z Has data issue: false hasContentIssue false
  • English
  • Français

Binarity of the LBV HR Car

Published online by Cambridge University Press:  23 January 2015

Th. Rivinius ,
H. M. J. Boffin ,
W. J. de Wit ,
A. Mehner ,
Ch. Martayan ,
S. Guieu  and
J.-B. Le Bouquin
Th. Rivinius
Affiliation:
ESO - European Organisation for Astronomical Research in the Southern Hemisphere, Chile email: [email protected]
H. M. J. Boffin
Affiliation:
ESO - European Organisation for Astronomical Research in the Southern Hemisphere, Chile email: [email protected]
W. J. de Wit
Affiliation:
ESO - European Organisation for Astronomical Research in the Southern Hemisphere, Chile email: [email protected]
A. Mehner
Affiliation:
ESO - European Organisation for Astronomical Research in the Southern Hemisphere, Chile email: [email protected]
Ch. Martayan
Affiliation:
ESO - European Organisation for Astronomical Research in the Southern Hemisphere, Chile email: [email protected]
S. Guieu
Affiliation:
Univ. Grenoble Alpes, CNRS, IPAG, France
J.-B. Le Bouquin
Affiliation:
Univ. Grenoble Alpes, CNRS, IPAG, France
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

VLTI/AMBER and VLTI/PIONIER observations of the LBV HR Car show an interferometric signature that could not possibly be explained by an extended wind, more or less symmetrically distributed around a single object. Instead, observations both in the Brγ line and the H-band continuum are best explained by two point sources (or alternatively one point source and one slightly extended source) at about 2 mas separation and a contrast ratio of about 1:5. These observations establish that HR Car is a binary, but further interpretation will only be possible with future observations to constrain the orbit. Under the assumption that the current separation is close to the maximum one, the orbital period can be estimated to be of the order of 5 years, similar as in the η Car system. This would make HR Car the second such LBV binary.

Keywords

stars: individual (HR Car)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Issue S307: New windows on massive stars: asteroseismology, interferometry, and spectropolarimetry , June 2014 , pp. 295 - 296
Copyright
Copyright © International Astronomical Union 2015 

References

Le Bouquin, J.-B., Berger, J.-P., Lazareff, B., et al. 2011, A&A 535, A67Google Scholar
Lobel, A., Groh, J. H., Martayan, C., et al. 2013, A&A 559, A16Google Scholar
Martayan, C., Lobel, A., Baade, D., et al. 2012, in Carciofi, A. C. & Rivinius, T. (eds.), Circumstellar Dynamics at High Resolution, Vol. 464 of Astronomical Society of the Pacific Conference Series, p. 293Google Scholar
Sana, H., de Mink, S. E., de Koter, A., et al. 2012, Science 337, 444CrossRefGoogle Scholar
Tallon-Bosc, I., Tallon, M., Thiébaut, E., et al. 2008, Vol. 7013 of Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, article ID 70131JGoogle Scholar