Intermediate-mass Black Holes’ Effects on Compact Object Binaries

Deme, Barnabás; Meiron, Yohai; Kocsis, Bence

doi:10.3847/1538-4357/ab7921

Cited by 16 publications

(5 citation statements)

References 72 publications

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“…, where r is the radial distance of the binary from the central mass (Hoang et al 2018;Deme et al 2020). Gravitational torques from the binary may clear a cavity in the surrounding gas distribution, as suggested by numerical simulations (Artymowicz & Lubow 1994;Armitage & Natarajan 2005).…”

Section: Disc-binary Interactionmentioning

confidence: 93%

Evolution of binary black holes in AGN accretion discs: Disc-binary interaction and gravitational wave emission

Ishibashi

Gröbner

2020

A&A

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Binary black hole (BBH) mergers are the primary sources of gravitational wave (GW) events detected by LIGO/Virgo. Binary black holes embedded in the accretion discs of active galactic nuclei (AGN) are possible candidates for such GW events. We have developed an idealised analytic model for the orbital evolution of BBHs in AGN accretion discs by combining the evolution equations of disc-binary interaction and GW inspiral. We investigated the coupled “disc+GW”-driven evolution of BBHs transitioning from the disc-driven regime at large orbital separations into the GW-driven regime at small separations. In this evolution channel, BBH mergers are accelerated by a combination of orbital decay and orbital eccentricity growth in the disc-dominated regime. We provide a quantification of the resulting merger timescale τmerger, and analyse its dependence on both the accretion disc and binary orbital parameters. By computing the evolution of the orbital eccentricity as a function of the GW frequency, we predict that most binaries in AGN discs should have significant residual eccentricities (e ∼ 0.01 − 0.1), potentially detectable by LISA. We further discuss the potentials and caveats of this particular BBH-in-AGN channel in the framework of binary evolutionary paths.

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Section: Disc-binary Interactionmentioning

confidence: 93%

Evolution of binary black holes in AGN accretion discs: Disc-binary interaction and gravitational wave emission

Ishibashi

Gröbner

2020

A&A

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“…(1 + e)( 3M SMBH M b ) 1/3 , where r is the radial distance of the binary from the central mass (Hoang et al 2018;Deme et al 2020). Gravitational torques from the binary may clear a cavity in the surrounding gas distribution, as suggested by numerical simulations (Artymowicz & Lubow 1994;Armitage & Natarajan 2005).…”

Section: Disc-binary Interactionmentioning

confidence: 95%

Evolution of binary black holes in AGN accretion discs: Disc-binary interaction and gravitational wave emission

Ishibashi,

Gröbner

2020

Preprint

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Binary black hole (BBH) mergers are the primary sources of gravitational wave (GW) events detected by LIGO/Virgo. Binary black holes embedded in the accretion discs of active galactic nuclei (AGN) are possible candidates for such GW events. We develop an idealised analytic model for the orbital evolution of BBHs in AGN accretion discs by combining the evolution equations of disc-binary interaction and GW inspiral. We investigate the coupled 'disc+GW'-driven evolution of BBHs transitioning from the disc-driven regime at large orbital separations into the GW-driven regime at small separations. In this evolution channel, BBH mergers are accelerated by a combination of orbital decay and orbital eccentricity growth in the disc-dominated regime. We provide a quantification of the resulting merger timescale τ merger , and analyse its dependence on both the accretion disc and binary orbital parameters. By computing the evolution of the orbital eccentricity as a function of the GW frequency, we predict that most binaries in AGN discs should have significant residual eccentricities (e ∼ 0.01 − 0.1), potentially detectable by LISA. We further discuss the potentials and caveats of this particular BBH-in-AGN channel in the framework of binary evolutionary paths.

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“…These putative IMBHs are supposedly harboured in a handful of compact gaseous clouds, whose measured velocity dispersion is so high to suggest the presence in their centres of point-like objects with masses in the range 10 4 -10 5 M (Oka et al, 2017;Takekawa et al, 2019Takekawa et al, , 2020. However, depending on their orbital properties, a population of IMBHs lurking at the Galactic Centre would affect significantly the motion of S-stars (Deme et al, 2020b) and the structure of the nuclear star cluster (Mastrobuono-Battisti et al, 2014).…”

Section: Heavy Imris From Galactic Nuclei Assemblymentioning

confidence: 99%

Astrophysics with the Laser Interferometer Space Antenna

Amaro-Seoane¹,

Andrews²,

Sedda³

et al. 2022

Preprint

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AM CVn binaries consist of a WD accreting from a hydrogen-deficient star (or WD) companion (Warner, 1995;Solheim, 2010). In their formation history (Fig. 1.6 and Section 1.3.1.1), AM CVns form after at least one CE phase of their progenitor system. The current RLO is initiated, due to orbital damping caused by GW radiation, at orbital periods of typically 5−20 min (depending on the nature and the temperature of the companion star), and the mass-transfer rate is determined

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Intermediate-mass Black Holes’ Effects on Compact Object Binaries

Cited by 16 publications

References 72 publications

Evolution of binary black holes in AGN accretion discs: Disc-binary interaction and gravitational wave emission

Evolution of binary black holes in AGN accretion discs: Disc-binary interaction and gravitational wave emission

Evolution of binary black holes in AGN accretion discs: Disc-binary interaction and gravitational wave emission

Astrophysics with the Laser Interferometer Space Antenna

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