Stellar and Dynamical Evolution within Triple Stars

Eggleton, P. P.; Kiseleva, L. G.

doi:10.1007/978-94-009-1673-9_17

Cited by 19 publications

(11 citation statements)

References 53 publications

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“…From the different evolutionary schemes of Eggleton & Kiseleva (1996), it is however unlikely that the third star has a giant luminosity class. Indeed, according to these authors, a massive triple system such as HD 150136, i.e., with M P > M S > M T , should first undergo a Roche lobe overflow in the inner binary.…”

Section: Evolutionary Statusmentioning

confidence: 99%

Evidence for a physically bound third component in HD 150136

Mahy

Gosset

Sana

et al. 2012

A&A

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Context. HD 150136 is one of the nearest systems harbouring an O3 star. Although this system was considered for a long time as a binary, more recent investigations have suggested the possible existence of a third component. Aims. We present a detailed analysis of HD 150136 to test its triple nature. In addition, we investigate the physical properties of the individual components of this system. Methods. We analysed high-resolution, high signal-to-noise data collected through multi-epoch runs spread over ten years. We applied a disentangling program to refine the radial velocities and to obtain the individual spectra of each star. With the radial velocities, we computed the orbital solution of the inner system, and we describe the main properties of the orbit of the outer star such as the preliminary mass ratio, the eccentricity, and the orbital-period range. With the individual spectra, we determined the stellar parameters of each star by means of the CMFGEN atmosphere code. Results. We offer clear evidence that HD 150136 is a triple system composed of an O3V((f * ))-3.5V((f + )), an O5.5-6V((f)), and an O6.5-7V((f)) star. The three stars are between 0-3 Myr old. We derive dynamical masses of about 64, 40, and 35 M for the primary, the secondary and the third components by assuming an inclination of 49 • (sin 3 i = 0.43). It currently corresponds to one of the most massive systems in our galaxy. The third star moves with a period in the range of 2950 to 5500 d on an outer orbit with an eccentricity of at least 0.3. However, because of the long orbital period, our dataset is not sufficient to constrain the orbital solution of the tertiary component with high accuracy. Conclusions. We confirm there is a tertiary star in the spectrum of HD 150136 and show that it is physically bound to the inner binary system. This discovery makes HD 150136 the first confirmed triple system with an O3 primary star.

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Section: Evolutionary Statusmentioning

confidence: 99%

Evidence for a physically bound third component in HD 150136

Mahy

Gosset

Sana

et al. 2012

A&A

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“…Typical examples of studies that focused on the three-body dynamics include Fabrycky and Tremaine (2007); Ford et al (2000); Liu et al (2015a); Naoz and Fabrycky (2014); Naoz et al (2013), and stellar evolution studies include Eggleton and Kiseleva (1996); Iben and Tutukov (1999); Kuranov et al (2001). Interdisciplinary studies, in which the mutual interaction between the dynamics and stellar aspects are taken into account are rare (Hamers et al, 2013;Kratter and Perets, 2012;Michaely and Perets, 2014;Naoz et al, 2016;Perets and Kratter, 2012;Shappee and Thompson, 2013), but demonstrate the richness of the interacting regime.…”

Section: Introductionmentioning

confidence: 99%

The evolution of hierarchical triple star-systems

2016

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Field stars are frequently formed in pairs, and many of these binaries are part of triples or even higher-order systems. Even though, the principles of single stellar evolution and binary evolution, have been accepted for a long time, the long-term evolution of stellar triples is poorly understood. The presence of a third star in an orbit around a binary system can significantly alter the evolution of those stars and the binary system. The rich dynamical behaviour in three-body systems can give rise to Lidov-Kozai cycles, in which the eccentricity of the inner orbit and the inclination between the inner and outer orbit vary periodically. In turn, this can lead to an enhancement of tidal effects (tidal friction), gravitational-wave emission and stellar interactions such as mass transfer and collisions. The lack of a self-consistent treatment of triple evolution, including both three-body dynamics as well as stellar evolution, hinders the systematic study and general understanding of the long-term evolution of triple systems. In this paper, we aim to address some of these hiatus, by discussing the dominant physical processes of hierarchical triple evolution, and presenting heuristic recipes for these processes. To improve our understanding on hierarchical stellar triples, these descriptions are implemented in a public source code TrES, which combines three-body dynamics (based on the secular approach) with stellar evolution and their mutual influences. Note that modelling through a phase of stable mass transfer in an eccentric orbit is currently not implemented in TrES, but can be implemented with the appropriate methodology at a later stage.

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“…W UMa-type systems have the least amount of angular momentum that binary stars can have and therefore they attract special attention as laboratories to test the angular momentum evolution of binary stars. Several reviews have discussed properties of W UMa-type systems; the recent ones, concentrating respectively on theoretical and observational issues, have been published by Eggleton (1996) and by Rucinski (1993a). A very recent catalogue of field contact binaries which have been compiled by is a good source for their physical parameters.…”

Section: Introductionmentioning

confidence: 99%

Key parameters of W UMa-type contact binaries discovered byHIPPARCOS

Selam

2004

A&A

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Abstract.A sample of W UMa-type binaries which were discovered by the HIPPARCOS satellite was constructed with the aid of well defined selection criteria described in this work. The selection process showed up that several systems of which the variability types have been assigned as EB in HIPPARCOS catalogue are genuine contact binaries of W UMa-type. The light curves of the 64 selected systems based on HIPPARCOS photometry were analyzed with the aid of light curve synthesis method by Rucinski and their geometric elements (namely mass ratio q, degree of contact f , and orbital inclination i) were determined. The solutions were obtained for the first time for many of the systems in the sample and would be a good source for their future light curve analyses based on more precise follow-up observations.

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Stellar and Dynamical Evolution within Triple Stars

Cited by 19 publications

References 53 publications

Evidence for a physically bound third component in HD 150136

Evidence for a physically bound third component in HD 150136

The evolution of hierarchical triple star-systems

Key parameters of W UMa-type contact binaries discovered byHIPPARCOS

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