Spin–Orbit Misalignment of Merging Black Hole Binaries with Tertiary Companions

Liu, Bin; Lai, Dong

doi:10.3847/2041-8213/aa8727

Cited by 90 publications

(98 citation statements)

References 36 publications

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“…If the beaming direction of pulse signal is changed, the pulsar will disappear in the stage B. However, following Liu & Lai (2017), we find that the adiabaticity, which measures the ratio of the KL oscillation time scale to the presession time scale, is very small in the present system. It means that the spin of the inner binary evolves "non-adiabatically" even when the KL-oscillation occurs.…”

Section: Resultsmentioning

confidence: 64%

Cumulative shift of periastron time of binary pulsar with Kozai–Lidov oscillation

Suzuki

Gupta

Okawa

et al. 2019

Monthly Notices of the Royal Astronomical Society: Letters

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We study a hierarchical triple system with the Kozai-Lidov mechanism, and analyse the cumulative shift of periastron time of a binary pulsar by the emission of gravitational waves. Time evolution of the osculating orbital elements of the triple system is calculated by directly integrating the first-order post-Newtonian equations of motion. The Kozai-Lidov mechanism will bend the evolution curve of the cumulative shift when the eccentricity becomes large. We also investigate the parameter range of mass and semi-major axis of the third companion with which the bending of the cumulative-shift curve could occur within 100 years.

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Section: Resultsmentioning

confidence: 64%

Cumulative shift of periastron time of binary pulsar with Kozai–Lidov oscillation

Suzuki

Gupta

Okawa

et al. 2019

Monthly Notices of the Royal Astronomical Society: Letters

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“…A similar result for T m , but neglecting singly-averaged effects 5 (i.e. with e max = e max ), has been previously used by several authors to calculate merger times of binaries driven to high eccentricity via the LK mechanism (Thompson 2011;Antonini & Perets 2012;Liu & Lai 2018;Grishin et al 2018;Randall & Xianyu 2018).…”

Section: Merger Time T Mmentioning

confidence: 73%

Compact Object Binary Mergers Driven By Cluster Tides: A New Channel for LIGO/Virgo Gravitational-wave Events

Hamilton¹,

Rafikov²

2019

ApJL

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The detections of gravitational waves produced in mergers of binary black holes (BH) and neutron stars (NS) by LIGO/Virgo have stimulated interest in the origin of the progenitor binaries. Dense stellar systems -globular and nuclear star clusters -are natural sites of compact object binary formation and evolution towards merger. Here we explore a new channel for the production of binary mergers in clusters, in which the tidal field of the cluster secularly drives the binary to high eccentricity (even in the absence of a central massive black hole) until gravitational wave emission becomes important. We employ the recently developed secular theory of cluster tide-driven binary evolution to compute present day merger rates for BH-BH, NS-BH and NS-NS binaries, varying cluster potential and central concentration of the binary population (but ignoring cluster evolution and stellar flybys for now). Unlike other mechanisms, this new dynamical channel can produce a significant number of mergers out to cluster-centric distances of several pc. For NS-NS binaries we find merger rates in the range 0.01 − 0.07 Gpc −3 yr −1 from globular clusters and 0.1 − 0.2 Gpc −3 yr −1 from cusped nuclear clusters. For NS-BH and BH-BH binaries we find small merger rates from globular clusters, but a rate of 0.1 − 0.2 Gpc −3 yr −1 from cusped nuclear clusters, contributing to the observed LIGO/Virgo rate at the level of several per cent. Therefore, cluster tide-driven mergers constitute a new channel that can be further explored with current and future gravitational wave detectors.

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“…As a weighted average of the mass and aligned spin of the binary, χ eff provides a convenient tool to test models of compact object binary spin properties via GW measurements [165][166][167][168][169][170]. Several authors suggest [171][172][173][174][175][176][177][178][179] how stellar binary evolutionary pathways leave imprints on the overall distribution of detected parameters such as masses and spins. By inferring the population properties of the events observed to date [55], we disfavor scenarios in which most black holes merge with large spins aligned with the binary's orbital angular momentum.…”

Section: Spinsmentioning

confidence: 99%

GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs

Abbott¹,

Abbott²,

Abbott³

et al. 2019

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We present the results from three gravitational-wave searches for coalescing compact binaries with component masses above 1 M ⊙ during the first and second observing runs of the advanced gravitationalwave detector network. During the first observing run (O1), from September 12, 2015 to January 19, 2016, gravitational waves from three binary black hole mergers were detected. The second observing run (O2), which ran from November 30, 2016 to August 25, 2017, saw the first detection of gravitational waves from a binary neutron star inspiral, in addition to the observation of gravitational waves from a total of seven binary black hole mergers, four of which we report here for the first time: GW170729, GW170809, GW170818, and GW170823. For all significant gravitational-wave events, we provide estimates of the source properties. The detected binary black holes have total masses between 18.6 þ3.2 −0.7 M ⊙ and 84.4 þ15.8 −11.1 M ⊙ and range in distance between 320 þ120 −110 and 2840 þ1400 −1360 Mpc. No neutron star-black hole mergers were detected. In addition to highly significant gravitational-wave events, we also provide a list of marginal event candidates with an estimated false-alarm rate less than 1 per 30 days. From these results over the first two observing runs, which include approximately one gravitational-wave detection per 15 days of data searched, we infer merger rates at the 90% confidence intervals of 110 − 3840 Gpc −3 y −1 for binary neutron stars and 9.7 − 101 Gpc −3 y −1 for binary black holes assuming fixed population distributions and determine a neutron star-black hole merger rate 90% upper limit of 610 Gpc −3 y −1 .

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Spin–Orbit Misalignment of Merging Black Hole Binaries with Tertiary Companions

Cited by 90 publications

References 36 publications

Cumulative shift of periastron time of binary pulsar with Kozai–Lidov oscillation

Cumulative shift of periastron time of binary pulsar with Kozai–Lidov oscillation

Compact Object Binary Mergers Driven By Cluster Tides: A New Channel for LIGO/Virgo Gravitational-wave Events

GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs

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