Gravitational waves from hierarchical triple systems with Kozai-Lidov oscillation

Gupta, Priti; Suzuki, Haruka; Okawa, Hirotada; Maeda, Kei Ichi

doi:10.1103/physrevd.101.104053

Cited by 41 publications

(38 citation statements)

References 79 publications

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“…In addition, we show that a significant fraction of the triples produced by GCs will have high eccentricity in the LISA frequency range. Works by Randall & Xianyu (2019), Hoang et al (2019), Deme et al (2020), Emami & Loeb (2020), and Gupta et al (2020) have shown the potential for LISA to be able to detect the peaks of the eKL oscillation. We also find that, since GW radiation is efficient in reducing the eccentricity of merging binaries, sub-hertz detectors such as the proposed DECIGO detector (Kawamura et al 2011) will be crucial to understand the contribution of GCs to the merger rate (see also .…”

Section: Discussionmentioning

confidence: 99%

Black Hole Mergers from Hierarchical Triples in Dense Star Clusters

Martinez

Fragione

Kremer

et al. 2020

ApJ

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Hierarchical triples are expected to be produced by the frequent binary-mediated interactions in the cores of globular clusters. In some of these triples, the tertiary companion can drive the inner binary to merger following large eccentricity oscillations, as a result of the eccentric Kozai-Lidov mechanism. In this paper, we study the dynamics and merger rates of black hole (BH) hierarchical triples, formed via binary-binary encounters in the CMC Cluster Catalog, a suite of cluster simulations with present-day properties representative of the Milky Way's globular clusters. We compare the properties of the mergers from triples to the other merger channels in dense star clusters, and show that triple systems do not produce significant differences in terms of mass and effective spin distribution. However, they represent an important pathway for forming eccentric mergers, which could be detected by LIGO-Virgo/Kamioka Gravitational-Wave Detector (LVK), and future missions such as LISA and the DECi-hertz Interferometer Gravitational wave Observatory. We derive a conservative lower limit for the merger rate from this channel of 0.35 Gpc −3 yr −1 in the local universe and up to~9% of these events may have a detectable eccentricity at LVK design sensitivity. Additionally, we find that triple systems could play an important role in retaining second-generation BHs, which can later merge again in the core of the host cluster. Unified Astronomy Thesaurus concepts: Astrophysical black holes (98); Black holes (162); Stellar mass black holes (1611); Gravitational wave astronomy (675); Gravitational wave detectors (676); Gravitational wave sources (677); Gravitational waves (678); Globular star clusters (656); Star clusters (1567); Trinary stars (1714)

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Section: Discussionmentioning

confidence: 99%

Black Hole Mergers from Hierarchical Triples in Dense Star Clusters

Martinez

Fragione

Kremer

et al. 2020

ApJ

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“…Finally (F) triple or higher-order stellar systems can also lead to the formation of BBHs (e.g. Silsbee & Tremaine 2017;Rodriguez & Antonini 2018;Gupta et al 2020;Toonen et al 2020). Within their uncertainties, almost all of these formation channels have been shown to have rate estimates consistent or marginally consistent with the empirical LVC rates.…”

Section: Introductionmentioning

confidence: 99%

The impact of mass-transfer physics on the observable properties of field binary black hole populations

Bavera

Fragos

Zevin

et al. 2021

A&A

146

176

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We study the impact of mass-transfer physics on the observable properties of binary black hole populations that formed through isolated binary evolution. We used the POSYDON framework to combine detailed MESA binary simulations with the COSMIC population synthesis tool to obtain an accurate estimate of merging binary black hole observables with a specific focus on the spins of the black holes. We investigate the impact of mass-accretion efficiency onto compact objects and common-envelope efficiency on the observed distributions of the effective inspiral spin parameter χeff, chirp mass Mchirp, and binary mass ratio q. We find that low common envelope efficiency translates to tighter orbits following the common envelope and therefore more tidally spun up second-born black holes. However, these systems have short merger timescales and are only marginally detectable by current gravitational-wave detectors as they form and merge at high redshifts (z ∼ 2), outside current detector horizons. Assuming Eddington-limited accretion efficiency and that the first-born black hole is formed with a negligible spin, we find that all non-zero χeff systems in the detectable population can come only from the common envelope channel as the stable mass-transfer channel cannot shrink the orbits enough for efficient tidal spin-up to take place. We find that the local rate density (z ≃ 0.01) for the common envelope channel is in the range of ∼17–113 Gpc−3 yr−1, considering a range of αCE ∈ [0.2, 5.0], while for the stable mass transfer channel the rate density is ∼25 Gpc−3 yr−1. The latter drops by two orders of magnitude if the mass accretion onto the black hole is not Eddington limited because conservative mass transfer does not shrink the orbit as efficiently as non-conservative mass transfer does. Finally, using GWTC-2 events, we constrained the lower bound of branching fraction from other formation channels in the detected population to be ∼0.2. Assuming all remaining events to be formed through either stable mass transfer or common envelope channels, we find moderate to strong evidence in favour of models with inefficient common envelopes.

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“…This can be accomplished with the detection of electromagnetic counterparts (e.g., Lee et al 2010;Tsang 2013), or through the detection of imprints on the GW waveform present with some merger channels. For instance, for some EKL-assisted mergers in GN, the gravitational pull of the SMBH on the merging binary can be detected in both LIGO and LISA due to induced GW phase shifts (Inayoshi et al 2017;Meiron et al 2017), and eccentricity variations (Hoang et al 2019;Randall & Xianyu 2019;Deme et al 2020;Emami & Loeb 2020;Gupta et al 2020).…”

Section: Discussionmentioning

confidence: 99%

Neutron Star–Black Hole Mergers from Gravitational-wave Captures

Hoang

Naoz

Kremer

2020

ApJ

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LIGO's third observing run (O3) has reported several neutron star-black hole (NSBH) merger candidates. From a theoretical point of view, NSBH mergers have received less attention in the community than either binary black holes, or binary neutron stars. Here we examine single-single (sin-sin) gravitational wave (GW) captures in different types of star clusters-galactic nuclei, globular clusters, and young stellar clusters-and compare the merger rates from this channel to other proposed merger channels in the literature. There are currently large uncertainties associated with every merger channel, making a definitive conclusion about the origin of NSBH mergers impossible. However, keeping these uncertainties in mind, we find that sin-sin GW capture is unlikely to significantly contribute to the overall NSBH merger rate. In general, it appears that isolated binary evolution in the field or in clusters, and dynamically interacting binaries in triple configurations, may result in a higher merger rate.

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Gravitational waves from hierarchical triple systems with Kozai-Lidov oscillation

Cited by 41 publications

References 79 publications

Black Hole Mergers from Hierarchical Triples in Dense Star Clusters

Black Hole Mergers from Hierarchical Triples in Dense Star Clusters

The impact of mass-transfer physics on the observable properties of field binary black hole populations

Neutron Star–Black Hole Mergers from Gravitational-wave Captures

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