Volume 634, February 2020
|Number of page(s)||53|
|Section||Stellar structure and evolution|
|Published online||19 February 2020|
The Tarantula Massive Binary Monitoring
III. Atmosphere analysis of double-lined spectroscopic systems⋆
Instituut voor Sterrenkunde, KU Leuven, Celestijnlaan 200D, Bus 2401, 3001 Leuven, Belgium
2 Departamento de Física, Universidade do Estado do Rio Grande do Norte, Mossoró, RN, Brazil
3 Departamento de Física, Universidade Federal do Rio Grande do Norte, UFRN, CP 1641, Natal, RN 59072-970, Brazil
4 Argelander-Institut für Astronomie der Universität Bonn, Auf dem Hügel 71, 53121 Bonn, Germany
5 Astronomical Institute Anton Pannekoek, Amsterdam University, Science Park 904, 1098 XH Amsterdam, The Netherlands
6 Center for Astrophysics, Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA
7 UK Astronomy Technology Centre, Royal Observatory Edinburgh, Blackford Hill, Edinburgh EH9 3HJ, UK
8 Département de Physique, Université de Montréal, and Centre de Recherche en Astrophysique de Québec, CP 6128, Succ. C-V, Montréal, QC H3C 3J7, Canada
9 Zentrum für Astronomie der Universität Heidelberg, Astronomisches Rechen-Institut, Mönchhofstr. 12-14, 69120 Heidelberg, Germany
10 Heidelberger Institut für Theoretische Studien, Schloss-Wolfsbrunnenweg 35, 69118 Heidelberg, Germany
11 Departamento de Física y Astronomía, Universidad de La Serena, Av. Cisternas 1200 Norte, La Serena, Chile
12 School of Physical Sciences, The Open University, Walton Hall, Milton Keynes MK7 6AA, UK
13 Dept. of Physics and Astronomy, University of Sheffield, Hounsfield Road, Sheffield S3 7RH, UK
14 Instituto de Astrofísica de Canarias, 38205 La Laguna, Tenerife, Spain
15 ESA, European Space Astronomy Centre, Apdo. de Correos 78, 28691 Villanueva de la Cañada, Madrid, Spain
16 IAASARS, National Observatory of Athens, 15326 Penteli, Greece
17 Armagh Observatory, College Hill, Armagh BT61 9DG, UK
Accepted: 3 December 2019
Context. Accurate stellar parameters of individual objects in binary systems are essential to constrain the effects of binarity on stellar evolution. These parameters serve as a prerequisite to probing existing and future theoretical evolutionary models.
Aims. We aim to derive the atmospheric parameters of the 31 double-lined spectroscopic binaries in the Tarantula Massive Binary Monitoring sample. This sample, composed of detached, semi-detached and contact systems with at least one of the components classified as an O-type star, is an excellent test-bed to study how binarity can impact our knowledge of the evolution of massive stars.
Methods. In the present paper, 32 epochs of FLAMES/GIRAFFE spectra are analysed by using spectral disentangling to construct the individual spectra of 62 components. We then apply the CMFGEN atmosphere code to determine their stellar parameters and their helium, carbon, and nitrogen surface abundances.
Results. Among the 31 systems that we study in the present paper, we identify between 48 and 77% of them as detached, likely pre-interacting systems, 16% as semi-detached systems, and between 5 and 35% as systems in or close to contact phase. Based on the properties of their components, we show that the effects of tides on chemical mixing are limited. Components on longer-period orbits show higher nitrogen enrichment at their surface than those on shorter-period orbits, in contrast to expectations of rotational or tidal mixing, implying that other mechanisms play a role in this process. For semi-detached systems, components that fill their Roche lobe are mass donors. They exhibit higher nitrogen content at their surface and rotate more slowly than their companions. By accreting new material, their companions spin faster and are likely rejuvenated. Their locations in the N − v sin i diagram tend to show that binary products are good candidates to populate the two groups of stars (slowly rotating, nitrogen-enriched objects and rapidly rotating non-enriched objects) that cannot be reproduced through single-star population synthesis. Finally, we find no peculiar surface abundances for the components in (over-)contact systems, as has been suggested by evolutionary models for tidal mixing.
Conclusions. This sample, consisting of 31 massive binary systems, is the largest sample of binaries composed of at least one O-type star to be studied in such a homogeneous way by applying spectral disentangling and atmosphere modelling. The study of these objects gives us strong observational constraints to test theoretical binary evolutionary tracks.
Key words: stars: early-type / binaries: spectroscopic / open clusters and associations: individual: 30 Doradus / stars: fundamental parameters
© ESO 2020
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