Common Proper Motion Companions to Nearby Stars: Ages and Evolution

Макаров, В. В.; Zacharias, N.; Hennessy, G. S.

doi:10.1086/591638

Cited by 53 publications

(52 citation statements)

References 91 publications

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“…In addition, the frequency of hierarchical triple systems among wide systems (separation ≥1000 AU) is also high (Makarov, Zacharias & Hennessy 2008). This suggests that the presence of an outer companion plays an important role in the formation of tight pairs, presumably through energy and angular momentum exchanges.…”

Section: High-order Multiple Systemsmentioning

confidence: 99%

Stellar Multiplicity

Duchêne

Kraus

2013

Annu. Rev. Astron. Astrophys.

1,311

1,285

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Stellar multiplicity is an ubiquitous outcome of the star formation process. Characterizing the frequency and main characteristics of multiple systems and their dependencies on primary mass and environment is therefore a powerful tool to probe this process. While early attempts were fraught with selection biases and limited completeness, instrumentation breakthroughs in the last two decades now enable robust analyses. In this review, we summarize our current empirical knowledge of stellar multiplicity for Main Sequence stars and brown dwarfs, as well as among populations of Pre-Main Sequence stars and embedded protostars. Clear trends as a function of both primary mass and stellar evolutionary stage are identified that will serve as a comparison basis for numerical and analytical models of star formation.

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Section: High-order Multiple Systemsmentioning

confidence: 99%

Stellar Multiplicity

Duchêne

Kraus

2013

Annu. Rev. Astron. Astrophys.

1,311

1,285

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“…Observationally, wide binaries are often found to be triple systems 8,9,48 . However, most wide binaries are not known to be triple systems 49 .…”

Section: Are All Wide Binaries Triple Systems?mentioning

confidence: 99%

Formation of the widest binary stars from dynamical unfolding of triple systems

Reipurth

Mikkola

2012

Nature

190

189

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“…Although binaries with separations larger than 10 000 au and up to 200,000 au have been reported in the literature (e.g. Makarov et al 2008;Quinn & Smith 2009;Poveda et al 2009;Raghavan et al 2010;Deacon et al 2012), most of these systems are either young or expected to be disrupted at older ages or are halo binaries. Another possibility is that these systems could be disrupted binaries that drift apart quite slowly because disruption does not necessarily denote a violent phenomenon, suggesting that these pairs would survive as common proper motion associations for much longer than their disruption time-scales (Shaya & Olling 2011).…”

Section: Stability Of Wide Companionsmentioning

confidence: 99%

Binary frequency of planet-host stars at wide separations

Lodieu

Pérez‐Garrido

Béjar

et al. 2014

A&A

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Aims. The aim of the project is to improve our knowledge on the multiplicity of planet-host stars at wide physical separations. Methods. We cross-matched approximately 6200 square degree area of the southern sky imaged by the Visible Infrared Survey Telescope for Astronomy (VISTA) Hemisphere Survey (VHS) with the Two Micron All Sky Survey (2MASS) to look for wide common proper motion companions to known planet-host stars. We complemented our astrometric search with photometric criteria. Results. We confirmed spectroscopically the co-moving nature of seven sources out of 16 companion candidates and discarded eight, while the remaining one stays as a candidate. Among these new wide companions to planet-host stars, we discovered a T4.5 dwarf companion at 6.3 arcmin (∼9000 au) from HIP 70849, a K7V star which hosts a 9 Jupiter mass planet with an eccentric orbit. We also report two new stellar M dwarf companions to one G and one metal-rich K star. We infer stellar and substellar binary frequencies for our complete sample of 37 targets of 5.4 ± 3.8% and 2.7 ± 2.7% (1σ confidence level), respectively, for projected physical separations larger than ∼60-160 au assuming the range of distances of planet-host stars (24-75 pc). These values are comparable to the frequencies of non planet-host stars. We find that the period-eccentricity trend holds with a lack of multiple systems with planets at large eccentricities (e > 0.2) for periods less than 40 days. However, the lack of planets more massive than 2.5 Jupiter masses and short periods (<40 days) orbiting single stars is not so obvious due to recent discoveries by ground-based transit surveys and space missions.

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Common Proper Motion Companions to Nearby Stars: Ages and Evolution

Cited by 53 publications

References 91 publications

Stellar Multiplicity

Stellar Multiplicity

Formation of the widest binary stars from dynamical unfolding of triple systems

Binary frequency of planet-host stars at wide separations

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