The Incidence of Multiplicity Among Bright Stellar Systems

Eggleton, P. P.; Kisseleva-Eggleton, Ludmila; Dearborn, Xander

doi:10.1017/s1743921307004280

Cited by 6 publications

(8 citation statements)

References 13 publications

(11 reference statements)

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“…The loser in AL Cam, for example, must have shed more than three quarters of its mass already, though the period is still only ∼1.33 d. In addition, the absence of a detectable secular increase in period implies that the EB is well-advanced in its evolution to an Algol, but perhaps three body dynamical interactions have inhibited the normal expansion of the close pair's orbit (cf. Eggleton et al 2007;Fabrycky & Tremaine 2007). The generally quite similar binary V338 Her, on the other hand, has a period increaseṖ of about 1.9 ×10 −7 d/yr.…”

Section: Discussionmentioning

confidence: 98%

A fresh insight into the evolutionary status and third body hypothesis of the eclipsing binaries AD Andromedae, AL Camelopardalis, and V338 Herculis

Liakos

Niarchos

Budding

2012

A&A

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Aims. We aim to derive the absolute parameters of the components of AD And, AL Cam, and V338 Her, interpret their orbital period changes and discuss their evolutionary status. Methods. New and complete multi-filter light curves of the eclipsing binaries AD And, AL Cam, and V338 Her were obtained and analysed with modern methods. Using all reliably observed times of minimum light, we examined orbital period irregularities using the least squares method. In addition, we acquired new spectroscopic observations during the secondary eclipses for AL Cam and V338 Her. Results. For AL Cam and V338 Her, we derive reliable spectral types for their primary stars. Statistical checks of orbital period analysis for all systems are very reassuring in the cases of V338 Her and AD And, although less so for AL Cam. The LIght-Time Effect (LITE) results are checked by inclusion of a third light option in the photometric analyses. Light curve solutions provide the means to calculate the absolute parameters of the components of the systems and reliably estimate their present evolutionary status. Conclusions. AL Cam and V338 Her are confirmed as classical Algols of relatively low mass in similar configurations. Unlike AL Cam, however, V338 Her is still transferring matter between its components, raising interest in the determinability of the evolutionary histories of Algols. AD And is found to be a detached system in which both close stars are of age ∼10 9 yr and is probably a "non-classical" young triple, at an interesting stage of its dynamical evolution.

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Section: Discussionmentioning

confidence: 98%

A fresh insight into the evolutionary status and third body hypothesis of the eclipsing binaries AD Andromedae, AL Camelopardalis, and V338 Herculis

Liakos

Niarchos

Budding

2012

A&A

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“…Triple systems are common in the Universe. They are found in many different astrophysical settings covering a large range of mass and physical scales, such as triple stars (e.g., Tokovinin 1997;Eggleton et al 2007;Tokovinin 2014b,a), and accreting compact binaries with a companion (such as companions to X-ray binaries e.g., Grindlay et al 1988;Prodan and Murray 2012). In addition, it seems that supermassive black hole binaries and higher multiples are common and thus, any star in their vicinity forms a triple system (e.g., Valtonen 1996;Di Matteo et al 2005;Khan et al 2012;Kulkarni and Loeb 2012).…”

Section: Introductionmentioning

confidence: 99%

The Eccentric Kozai-Lidov Effect and Its Applications

Naoz

2016

Annu. Rev. Astron. Astrophys.

664

564

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The hierarchical triple body approximation has useful applications to a variety of systems from planetary and stellar scales to supermassive black holes. In this approximation, the energy of each orbit is separately conserved and therefore the two semi-major axes are constants. On timescales much larger than the orbital periods, the orbits exchange angular momentum which leads to eccentricity and orientation (i.e., inclination) oscillations. The orbits' eccentricity can reach extreme values leading to a nearly radial motion, which can further evolve into short orbit periods and merging binaries. Furthermore, the orbits' mutual inclination may change dramatically from pure prograde to pure retrograde leading to misalignment and a wide range of inclinations. This dynamical behavior is coined as the "eccentric Kozai-Lidov" mechanism. The behavior of such a system is exciting, rich and chaotic in nature. Furthermore, these dynamics are accessible from a large part of the triple body parameter space and can be applied to diverse range of astrophysical settings and used to gain insights to many puzzles.Comment: 60 pages 25 figures, to appear in Annual Review of Astronomy and Astrophysics, comments welcom

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“…Many short period KGF binaries may in fact occur in a triple configuration (Tokovinin 1997;Pribulla & Rucinski 2006;Tokovinin 2008;Moe & Di Stefano 2017;Eggleton et al 2007;Griffin 2012). Similarly, massive binaries may often reside in triple configurations (Raghavan et al 2010;Zinnecker & Yorke 2007).…”

Section: Introductionmentioning

confidence: 99%

Companion-driven evolution of massive stellar binaries

Rose

Naoz

Geller

2019

Monthly Notices of the Royal Astronomical Society

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At least 70% of massive OBA-type stars reside in binary or higher-order systems. The dynamical evolution of these systems can lend insight into the origins of extreme phenomena such as X-ray binaries and gravitational wave sources. In one such dynamical process, the Eccentric Kozai-Lidov Mechanism, a third companion star alters the secular evolution of a binary system. For dynamical stability, these triple systems must have a hierarchical configuration. We explore the effects of a distant third companion's gravitational perturbations on a massive binary's orbital configuration before significant stellar evolution has taken place (≤ 10 Myr). We include tidal dissipation and general relativistic precession. With large (38, 000 total) Monte-Carlo realizations of massive hierarchical triples, we characterize imprints of the birth conditions on the final orbital distributions. Specifically, we find that the final eccentricity distribution over the range 0.1 − 0.7 is an excellent indicator of its birth distribution. Furthermore, we find that the period distributions have a similar mapping for wide orbits. Finally, we demonstrate that the observed period distribution for approximately 10 Myr-old massive stars is consistent with EKL evolution.

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The Incidence of Multiplicity Among Bright Stellar Systems

Cited by 6 publications

References 13 publications

A fresh insight into the evolutionary status and third body hypothesis of the eclipsing binaries AD Andromedae, AL Camelopardalis, and V338 Herculis

A fresh insight into the evolutionary status and third body hypothesis of the eclipsing binaries AD Andromedae, AL Camelopardalis, and V338 Herculis

The Eccentric Kozai-Lidov Effect and Its Applications

Companion-driven evolution of massive stellar binaries

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