Merger Rates of Intermediate-mass Black Hole Binaries in Nuclear Star Clusters

Fragione, Giacomo; Loeb, Abraham; Kocsis, Bence; Rasio, Frederic A.

doi:10.3847/1538-4357/ac75d0

Cited by 20 publications

(6 citation statements)

References 92 publications

(108 reference statements)

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“…Stellar systems with high central densities 10 5 pc −3 , such as globular clusters (GCs), have been claimed to yield optimal environments to form an IMBH either via sequential mergers of stellar-mass black holes (Coleman Miller & Hamilton 2002;Freitag et al 2006;Gürkan et al 2006;O'Leary et al 2006;Umbreit et al 2012;Rodriguez et al 2018;Antonini et al 2019;Rodriguez et al 2019;Fragione & Silk 2020;Mapelli et al 2021;Fragione et al 2022aFragione et al , 2022b or as a result of the collapse of a massive star from stellar collisions and mergers (Ebisuzaki et al 2001;Zwart & McMillan 2002;Gurkan et al 2004;Portegies Zwart et al 2004;Vanbeveren et al 2009;Banerjee 2020;Banerjee et al 2020;Kremer et al 2020;Das et al 2021;Di Carlo et al 2021;González et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Partial Tidal Disruptions of Main-sequence Stars by Intermediate-mass Black Holes

Kıroğlu

Lombardi

Kremer

et al. 2023

ApJ

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We study close encounters of a 1 M ⊙ middle-age main-sequence star (modeled using MESA) with massive black holes through hydrodynamic simulations, and explore in particular the dependence of the outcomes on the black hole mass. We consider here black holes in the intermediate-mass range, M BH = 100–104 M ⊙. Possible outcomes vary from a small tidal perturbation for weak encounters all the way to partial or full disruption for stronger encounters. We find that stronger encounters lead to increased mass loss at the first pericenter passage, in many cases ejecting the partially disrupted star on an unbound orbit. For encounters that initially produce a bound system, with only partial stripping of the star, the fraction of mass stripped from the star increases with each subsequent pericenter passage and a stellar remnant of finite mass is ultimately ejected in all cases. The critical penetration depth that separates bound and unbound remnants has a dependence on the black hole mass when M BH ≲ 103 M ⊙. We also find that the number of successive close passages before ejection decreases as we go from the stellar-mass black hole to the intermediate-mass black hole regime. For instance, after an initial encounter right at the classical tidal disruption limit, a 1 M ⊙ star undergoes 16 (5) pericenter passages before ejection from a 10 M ⊙ (100 M ⊙) black hole. Observations of periodic flares from these repeated close passages could in principle indicate signatures of a partial tidal disruption event.

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Section: Introductionmentioning

confidence: 99%

Partial Tidal Disruptions of Main-sequence Stars by Intermediate-mass Black Holes

Kıroğlu

Lombardi

Kremer

et al. 2023

ApJ

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“…Since isolated primordial stars are likely not accessible to JWST, small Population III galaxies and their integrated colors may provide the best opportunities for directly probing the properties of metal-free stars (Zackrisson et al 2011). Furthermore, thanks to their enhanced sensitivity, future ground-based (Einstein Telescope, Cosmic Explorer) and space-based (LISA, DECIGO) detectors are expected to collect gravitational-wave events from binary BH mergers in the range of ≈10 2 -10 4 M e up to a redshift of ≈20 (Fragione et al 2022;Saini et al 2022), a regime so far unexplored. In this perspective, theoretical studies of the evolution of primordial very massive stars are critical for contextualizing the upcoming data within an astrophysical picture.…”

Section: Discussionmentioning

confidence: 99%

A Study of Primordial Very Massive Star Evolution

Volpato¹,

Marigo²,

Costa

et al. 2023

ApJ

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We present new evolutionary models of primordial very massive stars with initial masses ranging from 100 to 1000 M ⊙ that extend from the main sequence to the onset of dynamical instability caused by the creation of electron–positron pairs during core C, Ne, or O burning, depending on the star’s mass and metallicity. Mass loss accounts for radiation-driven winds, as well as pulsation-driven mass loss on the main sequence and during the red supergiant phase. After examining the evolutionary properties, we focus on the final outcome of the models and associated compact remnants. Stars that avoid the pair instability supernova channel should produce black holes with masses ranging from ≈40 to ≈1000 M ⊙. In particular, stars with initial masses of about 100 M ⊙ could leave black holes of ≃85–90 M ⊙, values consistent with the estimated primary black hole mass of the GW190521 merger event. Overall, these results may contribute to explaining future data from next-generation gravitational-wave detectors, such as the Einstein Telescope and Cosmic Explorer, which will have access to an as-yet-unexplored black hole mass range of ≈102–104 M ⊙ in the early universe.

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“…For binaries consisting of two 100M BHs, the merger rate is smaller than 0.2 Gpc −3 yr −1 [98]. Merger rates have been proposed at the local universe due to repeated merges in dense stellar environments like globular and nuclear clusters [99][100][101][102][103], but these are mostly mergers of IMBHs with stellar mass BHs. In this work, we have focused on the merger of BHs of a similar mass.…”

Section: Cold Dark Matter Halosmentioning

confidence: 99%

Microlensing of gravitational waves by dark matter structures

Fairbairn

Urrutia

Vaskonen

2023

J. Cosmol. Astropart. Phys.

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Gravitational lensing of gravitational waves provides a potential new probe of dark matter structures. In this work, we consider the microlensing effect on gravitational wave signals from black hole binaries induced by low-mass dark matter halos that do not retain enough baryonic matter to hold stars. We clarify systematically when this microlensing effect is relevant and study in detail its detectability by future gravitational wave observatories. We consider lensing by cold dark matter halos and by solitonic cores that reside in fuzzy dark matter halos. Our results show that although the effect can be detectable at relatively large impact parameters, the probability of detecting such lensed events is low. In particular, we find that the expected number of events lensed by cold dark matter halos is 𝒪(0.01) per year for BBO and the expected number of events lensed by solitonic cores inside fuzzy dark matter halos is 𝒪(0.01) per year for ET. In the case that a significant fraction of dark matter consists of 𝒪(100 M ⊙) objects that are relatively compact, R < 𝒪(0.1 pc), we show that the expected number of lensed events per year for ET can be very large, 𝒪(1000).

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Merger Rates of Intermediate-mass Black Hole Binaries in Nuclear Star Clusters

Cited by 20 publications

References 92 publications

Partial Tidal Disruptions of Main-sequence Stars by Intermediate-mass Black Holes

Partial Tidal Disruptions of Main-sequence Stars by Intermediate-mass Black Holes

A Study of Primordial Very Massive Star Evolution

Microlensing of gravitational waves by dark matter structures

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