Volume 537, January 2012
|Number of page(s)||9|
|Section||Stellar structure and evolution|
|Published online||23 December 2011|
The VLT-FLAMES survey of massive stars: NGC 346-013 as a test case for massive close binary evolution⋆
1 Department of Physics and Astronomy, The Open University, Walton Hall, Milton Keynes MK7 6AA, UK
2 Lockheed Martin Integrated Systems, Building 1500, Langstone, Hampshire, PO9 1SA, UK
3 Faulkes Telescope Project, School of Physics and Astronomy, Cardiff University, Cardiff, CF24 3AA, UK
4 Division of Earth, Space and Environment, University of Glamorgan, Pontypridd, CF37 1DL, UK
5 UK Astronomy Technology Centre, Royal Observatory Edinburgh, Blackford Hill, Edinburgh, EH9 3HJ, UK
6 Department of Physics & Astronomy, Queen’s University Belfast, Belfast BT7 1NN, Northern Ireland, UK
7 ESA/STScI, 3700 San Martin Drive, Baltimore, MD 21218, USA
8 Argelander-Institut für Astronomie der Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
9 Astronomical Institute, Utrecht University, Princetonplein 5, Utrecht, The Netherlands
Received: 16 July 2011
Accepted: 20 October 2011
Context. NGC 346-013 is a peculiar double-lined eclipsing binary in the Small Magellanic Cloud (SMC) discovered by the VLT-FLAMES survey of massive stars.
Aims. We use spectroscopic and photometric observations to investigate the physical properties and evolutionary history of NGC 346-013.
Methods. Spectra obtained with VLT/FLAMES are used to construct a radial velocity curve for NGC 346-013 and to characterise the early B-type secondary. Photometry obtained with the Faulkes Telescope South is then used to derive orbital parameters, while spectra of the secondary are compared with synthetic spectra from TLUSTY model atmospheres.
Results. The orbital period is found to be 4.20381(12) days, with masses of 19.1 ± 1.0 and 11.9 ± 0.6 M⊙. The primary is a rapidly rotating (vrot = 320 ± 30 km s-1) late-O dwarf while the secondary, an early-B giant, displays near-synchronous rotation and has filled its Roche lobe, implying that it was originally the more massive component with recent mass transfer “spinning up” the primary to near-critical rotation. Comparison with synthetic spectra finds temperatures of 34.5 kK and 24.5 kK for the primary and secondary respectively, with the nitrogen abundance of the secondary enhanced compared to baseline values for the SMC, consistent with the predictions of models of interacting binaries.
Conclusions. NGC 346-013 likely evolved via non-conservative mass transfer in a system with initial masses ~22+15 M⊙, with the well-constrained orbital solution and atmospheric parameters making it an excellent candidate for tailored modelling with binary evolution codes. This system will form a cornerstone in constraining the physics of thermal timescale mass transfer, and the associated mass transfer efficiency, in massive close binary systems.
Key words: stars: early-type / stars: fundamental parameters / binaries: spectroscopic / Magellanic Clouds
© ESO, 2012
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