Volume 546, October 2012
|Number of page(s)||14|
|Published online||02 October 2012|
The 2.35 year itch of Cygnus OB2 #9
I. Optical and X-ray monitoring⋆,⋆⋆
1 Département AGO, Université de Liège, Allée du 6 Août 17, Bât. B5C, 4000 Liège, Belgium
2 Department of Physics & Astronomy, University of Wyoming, Laramie, WY 82071, USA
3 School of Physics and Astronomy, The University of Leeds, Woodhouse Lane, Leeds LS2 9JT, UK
4 Research School of Astronomy and Astrophysics, The Australian National University, Australia
5 Royal Observatory of Belgium, Ringlaan 3, 1180 Brussel, Belgium
Received: 19 April 2012
Accepted: 6 August 2012
Context. Nonthermal radio emission in massive stars is expected to arise in wind-wind collisions occurring inside a binary system. One such case, the O-type star Cyg OB2 #9, was proven to be a binary only four years ago, but the orbital parameters remained uncertain. The periastron passage of 2011 was the first one to be observable under good conditions since the discovery of binarity.
Aims. In this context, we have organized a large monitoring campaign to refine the orbital solution and to study the wind-wind collision.
Methods. This paper presents the analysis of optical spectroscopic data, as well as of a dedicated X-ray monitoring performed with Swift and XMM-Newton.
Results. In light of our refined orbital solution, Cyg OB2 #9 appears as a massive O+O binary with a long period and high eccentricity; its components (O5-5.5I for the primary and O3-4III for the secondary) have similar masses and similar luminosities. The new data also provide the first evidence that a wind-wind collision is present in the system. In the optical domain, the broad Hα line varies, displaying enhanced absorption and emission components at periastron. X-ray observations yield the unambiguous signature of an adiabatic collision, because as the stars approach periastron, the X-ray luminosity closely follows the 1/D variation expected in that case. The X-ray spectrum appears, however, slightly softer at periastron, which is probably related to winds colliding at slightly lower speeds at that time.
Conclusions. It is the first time that such a variation has been detected in O+O systems, and the first case where the wind-wind collision is found to remain adiabatic even at periastron passage.
Key words: binaries: spectroscopic / stars: early-type / stars: emission-line, Be / stars: individual: Cygnus OB2 #9 / X-rays: stars
Tables 1 and 2 are available in electronic form at http://www.aanda.org
© ESO, 2012
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