Orbits of new spectroscopic components in 7 multiple 
systems

Tokovinin, Andreï

doi:10.1051/aas:1997114

Cited by 47 publications

(46 citation statements)

References 5 publications

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“…Later it became evident that B and D are optical, whereas A and C share common proper motion. A was found to be a 3.8-day spectroscopic binary, C also turned out to be a spectroscopic binary with 3-day period (Tokovinin 1997a). This star is among the brightest in the sky in the far UV region of the spectrum because it hosts a young and hot white dwarf spatially coincident with C. Subsequent imaging with HST revealed that this WD is not identical to the spectroscopic secondary Cb, as one might expect, but is instead 2" away from C (Barstow et al 2001).…”

Section: Hierarchical or Sequential?mentioning

confidence: 93%

Designation of Multiple-star Components

Tokovinin

2005

Highlights astron.

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Abstract.Hierarchical multiple stars need designations for individual components, for super-components (several bodies that act as single dynamical center and are often measured jointly) and sub-systems. Hierarchical designations like those proposed for WMC can satisfy all needs, but designations will have to be frozen and will not reflect true hierarchy in the future as new components are discovered. Hence, a clearing house (WMC on the web?) is needed to maintain unique and consistent designations. The hierarchy can be coded separately and flexibly by reference to parent super-components. As an example, these ideas are applied to a real quintuple star HR 1706. W h a t and why designate?We are looking for a clear, unique and computer-friendly system for designating multiple stars and planets. We need to designate several different things. First, components -physical bodies like stars or planets. Second, super-componentsunions of several bodies that act as single dynamical centers. Some observational data (e.g. photometry, astrometry) refer to such combinations measured as a whole, without splitting into true components. Moreover, some components that are now believed to be single will be resolved in the future into sub-systems, so currently available data actually refer to super-components. Finally, we need designations for systems or sub-systems with approximately Keplerian orbits that are the building blocks of more complex stellar or planetary systems. Each system is composed of two components or super-components, which means that designations for systems can be derived from designations of their components. In the following we designate systems by joining two component's designations with comma.

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Section: Hierarchical or Sequential?mentioning

confidence: 93%

Designation of Multiple-star Components

Tokovinin

2005

Highlights astron.

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“…Indeed, the possible close visual component located at about 1.6 could be also bound to the system. In order to determine whether HD 150136 is a dynamically stable hierarchical triple system, we use the stability criterion quoted by Tokovinin (2004):…”

Section: The Tertiary Componentmentioning

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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“…Data processing, estimation of the measurement errors and their analysis are described in (Tokovinin 1992(Tokovinin , 1997a. Briefly, internal error of each measurement is estimated as σ…”

Section: Observationsmentioning

confidence: 99%

“…Precise measurement of the radial velocity difference between the components of long-period visual pairs was required for the computation of orbits by the dynamical method of Kiselev & Kiyaeva (1980). Initial results of such measurements, started in 1986, were published in Tokovinin (1994a); data on additional objects are given here. In some pairs from the Kiselev program the spectroscopic sub-systems were discovered and they were included in MSC.…”

Section: Introductionmentioning

confidence: 99%

Statistics of spectroscopic sub-systems in visual multiple stars

Tokovinin

Smekhov²

2002

A&A

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135

126

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Abstract.A large sample of visual multiples of spectral types F5-M has been surveyed for the presence of spectroscopic sub-systems. Some 4200 radial velocities of 574 components were measured in 1994-2000 with the correlation radial velocity meter. A total of 46 new spectroscopic orbits were computed for this sample. Physical relations are established for most of the visual systems and several optical components are identified as well. The period distribution of sub-systems has a maximum at periods from 2 to 7 days, likely explained by a combination of tidal dissipation with triple-star dynamics. The fraction of spectroscopic sub-systems among the dwarf components of close visual binaries with known orbits is similar to that of field dwarfs, from 11% to 18% per component. Sub-systems are more frequent among the components of wide visual binaries and among wide tertiary components to the known visual or spectroscopic binaries -20% and 30%, respectively. In triple systems with both outer (visual) and inner (spectroscopic) orbits known, we find an anti-correlation between the periods of inner sub-systems and the eccentricities of outer orbits which must be related to dynamical stability constraints.

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Orbits of new spectroscopic components in 7 multiple systems

Cited by 47 publications

References 5 publications

Designation of Multiple-star Components

Designation of Multiple-star Components

Evidence for a physically bound third component in HD 150136

Statistics of spectroscopic sub-systems in visual multiple stars

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