MOCCA-SURVEY Database - I. Coalescing binary black holes originating from globular clusters

By A. Askar, M. Szkudlarek, D. Gondek-Rosi'nska, M. Giersz, T. Bulik. 2016

252 citations recorded by the source corpus.

In this first of a series of papers, we utilize results for around two thousand star cluster models simulated using the MOCCA code for star cluster evolution (Survey Database I) to determine the astrophysical properties and local merger rate densities for coalescing binary black holes (BBHs) originating from globular clusters (GCs). We extracted information for all coalescing BBHs that escape the cluster models and subsequently merge within a Hubble time along with BBHs that are retained in our GC models and merge inside the cluster via gravitational wave (GW) emission. By obtaining results from a substantial number of realistic star cluster models that cover different initial parameters, we have an extremely large statistical sample of BBHs with stellar mass and massive stellar BH ($\lesssim 100M_{\odot}$) components that merge within a Hubble time. Using this data, we estimate local merger rate densities for these BBHs originating from GCs to be at least 5.4 ${\rm Gpc}^{-3}\,{\rm yr}^{-1}$

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/245441430d912f63af8dbf23494a517b10bad68c

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In Astronomy and Astrophysics

Citations in the corpus

Merging black holes in young star clusters (2019, background): “…Mapelli & Zampieri 2014; Ziosi et al. 2014; Rodriguez et al. 2015, 2016; Antonini & Rasio 2016; Mapelli 2016; Kimpson et al. 2016; Hurley et al. 2016; O’Leary et al. 2016; Askar et al. 2017, 2018; Zevin et al. 2017; Samsing 2018; Rodriguez et al. 2018; Antonini et al. 2018; Rastello et al. 2018).”
The cosmic merger rate of stellar black hole binaries from the Illustris simulation (2017, background): “Dynamical exchanges might lead to the formation of additional BHBs, which are likely more massive and more eccentric than average (e.g. Downing et al. 2010; Ziosi et al. 2014; Askar et al. 2017; Rodriguez et al. 2016; Banerjee 2017).”
Black hole growth through hierarchical black hole mergers in dense star clusters: implications for gravitational wave detections (2018, methodology): “…based on Monte Carlo and N-body techniques (e.g., Zwart & McMillan 1999; Downing et al. 2010; Banerjee et al. 2010; Rodriguez et al. 2015, 2016; Askar et al. 2017; Samsing et al. 2018) have shown that such dynamically formed binaries could explain many, or perhaps even most, of the BH mergers…”
Black Hole Mergers From Globular Clusters Observable by LISA I: Eccentric Sources Originating From Relativistic N-body Dynamics (2018, methodology): “We note here that these two distributions are in full agreement with those found in Samsing et al. (2018a), in which the distributions were resolved using full numerical 2.5 PN scatterings using data from the MOCCA code (Giersz et al. 2013; Askar et al. 2017).”
Merging black hole binaries with the SEVN code (2018, background): “In contrast, they can be very important if they form in star clusters, where they have a high chance to acquire a companion through dynamical exchanges, so that they possibly become loud GW sources (Portegies Zwart & McMillan 2000; Mapelli 2016; Askar et al. 2017).”
A catalogue of masses, structural parameters, and velocity dispersion profiles of 112 Milky Way globular clusters (2018, methodology): “The Monte Carlo simulations of Askar et al. (2017) assumed a point-mass galaxy with the same circular velocity.”
Evolutionary roads leading to low effective spins, high black hole masses, and O1/O2 rates for LIGO/Virgo binary black holes (2017, background): “…& Downing 2013; Bae et al. 2014; Chatterjee et al. 2017; Mapelli 2016; Hurley et al. 2016; Rodriguez et al. 2016a; VanLandingham et al. 2016; Askar et al. 2017; Arca-Sedda & Capuzzo-Dolcetta 2019; Samsing 2018; Morawski et al. 2018; Banerjee 2018; Di Carlo et al. 2019; Zevin et al. 2019;…”