Reference : Fundamental parameters of massive stars in multiple systems: The cases of HD 17505A a...
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/225662
Fundamental parameters of massive stars in multiple systems: The cases of HD 17505A and HD 206267A
English
Raucq, Françoise mailto [Space sciences, Technologies and Astrophysics Research (STAR) Institute, Université de Liège, Allée du 6 Août 19c, Bât. B5c, 4000, Liège, Belgium]
Rauw, Grégor mailto [Université de Liège - ULiège > > Groupe d'astrophysique des hautes énergies (GAPHE) >]
Mahy, Laurent mailto [Université de Liège - ULiège > Département d'astrophys., géophysique et océanographie (AGO) > Astroph. extragalactique et observations spatiales (AEOS) >]
Simón-Díaz, S. [Instituto de Astrofísica de Canarias, 38200, La Laguna, Tenerife, Spain; Departamento de Astrofísica, Universidad de La Laguna, 38205, La Laguna, Tenerife, Spain)]
1-Jun-2018
Astronomy and Astrophysics
EDP Sciences
614
Yes (verified by ORBi)
International
0004-6361
1432-0746
Les Ulis
France
[en] stars: early-type ; binaries: spectroscopic ; stars: fundamental parameters ; stars: massive ; stars: individual: HD17505 ; stars: individual: HD206267
[en] Context. Many massive stars are part of binary or higher multiplicity systems. The present work focusses on two higher multiplicity systems: HD 17505A and HD 206267A. <BR /> Aims: Determining the fundamental parameters of the components of the inner binary of these systems is mandatory to quantify the impact of binary or triple interactions on their evolution. <BR /> Methods: We analysed high-resolution optical spectra to determine new orbital solutions of the inner binary systems. After subtracting the spectrum of the tertiary component, a spectral disentangling code was applied to reconstruct the individual spectra of the primary and secondary. We then analysed these spectra with the non-LTE model atmosphere code CMFGEN to establish the stellar parameters and the CNO abundances of these stars. <BR /> Results: The inner binaries of these systems have eccentric orbits with e 0.13 despite their relatively short orbital periods of 8.6 and 3.7 days for HD 17505Aa and HD 206267Aa, respectively. Slight modifications of the CNO abundances are found in both components of each system. The components of HD 17505Aa are both well inside their Roche lobe, whilst the primary of HD 206267Aa nearly fills its Roche lobe around periastron passage. Whilst the rotation of the primary of HD 206267Aa is in pseudo-synchronization with the orbital motion, the secondary displays a rotation rate that is higher. <BR /> Conclusions: The CNO abundances and properties of HD 17505Aa can be explained by single star evolutionary models accounting for the effects of rotation, suggesting that this system has not yet experienced binary interaction. The properties of HD 206267Aa suggest that some intermittent binary interaction might have taken place during periastron passages, but is apparently not operating anymore. Based on observations collected with the TIGRE telescope (La Luz, Mexico), the 1.93 m telescope at Observatoire de Haute Provence (France), the Nordic Optical Telescope at the Observatorio del Roque de los Muchachos (La Palma, Spain), and the Canada-France-Hawaii telescope (Mauna Kea, Hawaii).
Space sciences, Technologies and Astrophysics Research - STAR
FRS/FNRS Research Project (T.0100.15), ARC "Etoiles massives"
Researchers ; Students
http://hdl.handle.net/2268/225662
10.1051/0004-6361/201732376
http://adsabs.harvard.edu/abs/2018A%26A...614A..60R

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