Merging compact binaries in hierarchical triple systems: Resonant excitation of binary eccentricity

Liu, Bin; Lai, Dong; Yuan, Ye‐Fei

doi:10.1103/physrevd.92.124048

Cited by 16 publications

(3 citation statements)

References 40 publications

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“…of three-body systems that we describe in this article. Indeed, it is known that octupolar terms can drastically alter the KL mechanism [25] or lead to another kind of precession resonance [27,28], while 1PN terms induced by the outer binary can be important when the third body is supermassive [38,40]. Can the inclusion of higher-order terms in the Hamiltonian 1 change the resonance behavior?…”

Section: Discussionmentioning

confidence: 99%

“…The purpose of this article is to study the effects of such kind of resonance, which we term by "precession resonance". Note that it is a phenomenon distinct from the "tidal res-onances" recently unveiled in [6,7], or from another kind of precession resonance where the precession timescales of both inner and outer orbits are commensurate, discussed in [27,28]. Although the consequences of a similar type of resonance have already been studied in the Solar system (the ν 6 resonance between asteroids and Saturn [29,30], however in this case the precession is not due to GR effects), we are not aware of any previous study of the impact of precession resonances on relativistic three-body systems.…”

Section: Introductionmentioning

confidence: 92%

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Precession resonances in hierarchical triple systems

Kuntz

2021

Preprint

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We describe a new kind of resonance occuring in relativistic three-body hierarchical systems: the precession resonance, occuring when the relativistic precession timescale of a binary equals the period of a distant perturber. We find that, contrary to what most previous studies assume, it can lead to an exponential increase of eccentricity of the binary even when relativistic precession dominates the quadrupolar perturbation. The resonance may happen in the observation band of LISA or change the eccentricity distribution of triples. We discuss the physics of the resonance, showing that it mainly depends on three parameters.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 92%

Precession resonances in hierarchical triple systems

Kuntz

2021

Preprint

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“…Previous studies have revealed that general relativity (GR) may have an influence on triples' evolution, which may result in resonant-like dynamics (Naoz et al 2013;Liu et al 2015) or destabilize the existing resonance (Hansen & Naoz 2020). We conduct additional runs by considering the GR effect with the same initials in Figure 4.…”

Section: Numerical Setupmentioning

confidence: 99%

Evolution of Planetary Obliquity: The Eccentric Kozai–Lidov Mechanism Coupled with Tide

Huang,

Ji,

Liu

et al. 2023

ApJ

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Planetary obliquity plays a significant role in determining the physical properties of planetary surfaces and climate. As direct detection is constrained due to the present observation accuracy, kinetic theories are helpful for predicting the evolution of planetary obliquity. Here the coupling effect between the eccentric Kozai–Lidov effect and the equilibrium tide is extensively investigated; the planetary obliquity is observed to follow two kinds of secular evolution paths, based on the conservation of total angular momentum. The equilibrium timescale of the planetary obliquity t eq varies along with r t , which is defined as the initial timescale ratio of the tidal dissipation and secular perturbation. We numerically derive the linear relationship between t eq and r t with the maximum likelihood method. The spin-axis orientation of S-type terrestrials orbiting M-dwarfs reverses over 90° when r t > 100, then enters the quasi-equilibrium state between 40° and 60°, while the maximum obliquity can reach 130° when r t > 104. Numerical simulations show that the maximum obliquity increases with the semimajor axis ratio a 1/a 2, but is not so sensitive to the eccentricity e 2. The likelihood of an obliquity flip for S-type terrestrials in general systems with a 2 < 45 au is closely related to m 1. The observed potentially oblique S-type planets HD 42936 b, GJ 86 Ab, and τ Boo Ab are explored and found to have a great possibility of rotating head-down over the secular evolution of spin.

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Wolf–Rayet stars, black holes and the first detected gravitational wave source

et al. 2018

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The recently discovered burst of gravitational waves GW150914 provides a good new chance to verify the current view on the evolution of close binary stars. Modern population synthesis codes help to study this evolution from two main sequence stars up to the formation of two final remnant degenerate dwarfs, neutron stars or black holes (Masevich & Tutukov, 1988). To study the evolution of the GW150914 predecessor we use the "Scenario Machine" code presented by Lipunov, Postnov & Prokhorov (1996). The scenario modelling conducted in this study allowed to describe the evolution of systems for which the final stage is a massive BH+BH merger. We find that the initial mass of the primary component can be 100 ÷ 140M ⊙ and the initial separation of the components can be 50 ÷ 350R ⊙ . Our calculations show the plausibility of modern evolutionary scenarios for binary stars and the population synthesis modelling based on it.

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Merging compact binaries in hierarchical triple systems: Resonant excitation of binary eccentricity

Cited by 16 publications

References 40 publications

Precession resonances in hierarchical triple systems

Precession resonances in hierarchical triple systems

Evolution of Planetary Obliquity: The Eccentric Kozai–Lidov Mechanism Coupled with Tide

Wolf–Rayet stars, black holes and the first detected gravitational wave source

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