Observational signatures of past mass-exchange episodes in massive binaries: The case of HD 149 404

Context. Mass and momentum exchanges in close massive binaries play an important role in their evolution, and produce several observational signatures such as asynchronous rotation and altered chemical compositions, that remain after the stars detach again. Aims: We investigated these effects for the detached massive O-star binary HD 149 404 (O7.5 If + ON9.7 I, P = 9.81 days), which is thought to have experienced a past episode of case A Roche-lobe overflow (RLOF). Methods: Using phase-resolved spectroscopy, we performed the disentangling of the optical spectra of the two stars. The reconstructed primary and secondary spectra were then analysed with the CMFGEN model atmosphere code to determine stellar parameters, such as the effective temperatures and surface gravities, and to constrain the chemical composition of the components. We complemented the optical study with the study of IUE spectra, which we compare to the synthetic binary spectra. The properties of the stars were compared to evolutionary models. Results: We confirmed a strong overabundance in nitrogen ([N/C] ~ 150[N/C][SUB]⊙[/SUB]) for the secondary and a slight nitrogen overabundance ([N/C] ~ 5[N/C][SUB]⊙[/SUB]) for the primary star. Comparing the two stars, we found evidence for asynchronous rotation, with a rotational period ratio of 0.50 ± 0.11. Conclusions: The hypothesis of a past case A RLOF interaction in HD 149 404 is most plausible to explain its chemical abundances and rotational asynchronicity. Some of the observed properties, such as the abundance pattern, are clearly a challenge for current case A binary evolution models, however.ARC - Actions de recherche concertées; Etoiles massive

Search for the signatures of mass-exchange episodes in massive binaries

Massive stars are known for their crucial role in our Universe, through their extreme stellar parameters, leading to a strong impact on their environment. However, there remain numbers of unanswered questions concerning the exact processes of their formation, their stability or the processes driving their strong stellar winds. In the context of this thesis work, we adress one of the most interesting of their peculiarities: their tendency to be part of binary of higher multiplicity systems. Whilst this multiplicity does help to solve some open issues by allowing us to study some of the fundamental properties of the stars, such as their minimum masses and radii as well as their stellar luminosities, it can also lead to interactions between the components of a system, which affect the subsequent evolution of the stars and give rise to additional open questions on the processes in place in such systems. Among the possible interactions taking place within close binary systems is the possibility of a transfer of mass and kinetic momentum through a Roche lobe overflow. This process has a huge impact on the subsequent evolution of both components and many aspects of this phenomenon are not well understood yet. The present work is devoted to the search for the signatures of such past mass-exchange episodes in a sample of four short-period massive multiple systems: HD 149404, LSS 3074, HD 17505 and HD 206267. We determined a new orbital solution for three of them. We then used phase-resolved spectroscopy to perform the spectral disentangling of the optical spectra of the components. The spectral disentangling is a mathematical tool which allows to separate the contributions of both components to the observed spectra of a system. We then analysed the reconstructed spectra with the CMFGEN atmosphere code to determine stellar parameters, such as the effective temperatures and surface gravities, and to constrain the surface chemical composition of each component. The first two parts of this dissertation are dedicated to the scientific background and the description of the numerical tools and methods used in this work. The third part presents our studies of the selected massive systems. We confirmed that the hypothesis of a past Roche lobe overflow episode is most plausible to explain the observed properties of the components of HD 149404. Photometric data permitted us to confirm that LSS 3074 is in an overcontact configuration, and a combined analysis with spectroscopy showed that the system has lost a significant fraction of its mass to its surroundings. We proposed several possible evolutionary pathways involving a Roche lobe overflow process to explain the current parameters of its components. We found no evidence of past mass-transfer episodes in the spectra of HD 17505 and showed that the current properties of its components can be explained by single star evolutionary models including rotational mixing. We found clues of binary interactions in the spectra of HD 206267, but suggested that the system did not experience a complete Roche lobe overflow episode at this stage of its evolution

Observational signatures of past mass-exchange episodes in massive binaries : The cases of HD17505 and HD206267

Mass and angular momentum exchanges through Roche Lobe Overflow interactions within close massive binaries are known to play an important role in the subsequent evolution of the components of such systems, and produce several observational signatures, such as asynchronous rotation and altered chemical compositions, that remain once the stars detach again. We have started to investigate these effects in a sample of massive O-star binaries that are thought to have previously experienced a Case A Roche Lobe Overflow episode. Using phase-resolved spectroscopy, we perform the disentangling of the optical spectra of the two stars. The reconstructed primary and secondary spectra are then analysed with the CMFGEN model atmosphere code to determine stellar parameters such as the effective temperatures, surface gravities and rotational velocities, and to constrain the chemical composition of the components. In this contribution, we present the results of our analyses of the triple system HD17505 ([O7V + O7V, P = 8.57 days] + O6.5III). We also present the first results of our analyses of the triple system HD206267 ([O6.5V + O9.5V,P = 3.71 days] + OB).ARC - Actions de Recherche Concertées; Etoiles massive

Observational signatures of past mass-exchange episodes in massive binaries : The cases of LSS 3074 and HD 17505

Mass and angular momentum exchanges through Roche Lobe Overflow interactions within close massive binaries are known to play an important role in the subsequent evolution of the components of such systems, and produce several observational signatures, such as asynchronous rotation and altered chemical compositions, that remain once the stars detach again. We have started to investigate these effects in a sample of massive O-star binaries that are thought to have previously experienced a Case A Roche Lobe Overflow episode. Using phase-resolved spectroscopy, we perform the disentangling of the optical spectra of the two stars. The reconstructed primary and secondary spectra re then analysed with the CMFGEN model atmosphere code to determine stellar parameters such as the effective temperatures, surface gravities and rotational velocities, and to constrain the chemical composition of the components. In this contribution, we present the results of our analyses of LSS 3074 (O5.5I + O6.5-7I, P = 2.1852 days), together with the analyses of its photometric lightcurve and orbital solution. We also present the first results of our analyses of the triple system HD17505 ([O7.5V + O7.5V, P = 8.57 days] + O6.5III).ARC - Actions de Recherche Concertées; Etoiles massive

Observational signatures of past mass-exchange episodes in massive binaries

Mass and momentum exchanges in massive binaries can produce several observational signatures, such as asynchronous rotation and altered chemical compositions, which remain once the stars detach again. We have started to investigate these effects for a sample of detached massive O-star binaries that are thought to have previously experienced a Case A Roche lobe overflow. Using phase-resolved spectroscopy, we perform the disentangling of the spectra of the two stars. The reconstructed primary and secondary spectra are then analyzed to determine a range of stellar effective temperatures and gravity, as well as rotational velocities. Using model atmosphere codes we also constrain the chemical composition of the components. In this contribution, we present the first results of our analyses of HD149404 (O7.5If + ON9.5I, P = 9.81 days)

Observational signatures of past mass-exchange episodes in massive binaries: The cases of HD 149 404 and HD 17505

Mass and momentum exchanges in close massive binaries play an important role in the evolution of such systems and produce several observational signatures, such as asynchronous rotation and altered chemical compositions, that remain once the stars detach again. We have started to investigate these effects for a sample of detached massive O-star binaries that are thought to have previously experienced a Case A Roche Lobe Overflow. Using phase-resolved spectroscopy, we perform the disentangling of the spectra of the two stars. The reconstructed primary and secondary spectra are then analyzed to determine a range of stellar effective temperatures and gravity, and rotational velocities. Using model atmosphere codes we also constrain the chemical composition of the components. In this contribution, we present the results of our analyses of HD149404 (O7.5If + ON9.5I, P = 9.81 days) and the first results of our analyses of HD17505 ([O7.5V + O7.5V, P = 8.57 days] + O6.5III).ARC - Actions de Recherche Concertées; Etoiles massive

BRITE photometry of the massive post-RLOF system HD149 404

Context. HD 149 404 is an evolved non-eclipsing O-star binary that has previously undergone a Roche lobe overflow interaction. Aims: Understanding some key properties of the system requires a determination of the orbital inclination and of the dimensions of the components. Methods: The BRITE-Heweliusz satellite was used to collect photometric data of HD 149 404. Additional photometry was retrieved from the SMEI archive. These data were analysed using a suite of period search tools. The orbital part of the lightcurve was modelled with the nightfall binary star code. The Gaia-DR2 parallax of HD 149 404 was used to provide additional constraints. Results: The periodograms reveal a clear orbital modulation of the lightcurve with a peak-to-peak amplitude near 0.04 mag. The remaining non-orbital part of the variability is consistent with red noise. The lightcurve folded with the orbital period reveals ellipsoidal variations, but no eclipses. The minimum when the secondary star is in inferior conjunction is deeper than the other minimum due to mutual reflection effects between the stars. Combined with the Gaia-DR2 parallaxes, the photometric data indicate an orbital inclination in the range of 23°-31° and a Roche lobe filling factor of the secondary larger than or equal to 0.96. Conclusions: The luminosity of the primary star is consistent with its present-day mass, whereas the more evolved secondary appears overluminous for its mass. We confirm that the primary's rotation period is about half the orbital period. Both features most probably stem from the past Roche lobe overflow episode. Based on data collected by the BRITE-Constellation satellite mission, designed, built, launched, operated and supported by the Austrian Research Promotion Agency (FFG), the University of Vienna, the Technical University of Graz, the University of Innsbruck, the Canadian Space Agency (CSA), the University of Toronto Institute for Aerospace Studies (UTIAS), the Foundation for Polish Science & Technology (FNiTP MNiSW), and the National Science Centre (NCN)