Dynamics of stellar black holes in young star clusters with different metallicities – II. Black hole–black hole binaries

By B. M. Ziosi, Michela Mapelli, M. Branchesi, G. Tormen. 2014

194 citations recorded by the source corpus.

In this paper, we study the formation and dynamical evolution of black hole-black hole (BH-BH) binaries in young star clusters (YSCs), by means of N-body simulations. The simulations include metallicity-dependent recipes for stellar evolution and stellar winds, and have been run for three different metallicities (Z = 0.01, 0.1 and 1 Zsun). Following recent theoretical models of wind mass-loss and core-collapse supernovae, we assume that the mass of the stellar remnants depends on the metallicity of the progenitor stars. We find that BH-BH binaries form efficiently because of dynamical exchanges: in our simulations, we find about 10 times more BH-BH binaries than double neutron star binaries. The simulated BH-BH binaries form earlier in metal-poor YSCs, which host more massive black holes (BHs) than in metal-rich YSCs. The simulated BH-BH binaries have very large chirp masses (up to 80 Msun), because the BH mass is assumed to depend on metallicity, and because BHs can grow in mass due to the merger with stars. The simulated BH-BH binaries span a wide range of orbital periods (10^-3-10^7 yr), and only a small fraction of them (0.3 per cent) is expected to merge within a Hubble time. We discuss the estimated merger rate from our simulations and the implications for Advanced VIRGO and LIGO.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/2bc3ae6a09b581802ccc7f80add8c9bdc204ea0d

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In Astronomy and Astrophysics

1. Michela Mapelli
2. N. Giacobbo
3. Ilya Mandel
4. Mario Spera
5. D. Holz
6. F. Rasio
7. Maya Fishbach
8. F. Antonini

Citations in the corpus

• Stellar-mass black holes in young massive and open stellar clusters and their role in gravitational-wave generation (2016, background): “2.2), for shorter evolutionary times of ∼ 100 Myr, to study the dynamical interactions involving BHs over young ages and low metallicities (Mapelli et al. 2013; Ziosi et al. 2014).”
• ASTROPHYSICAL IMPLICATIONS OF THE BINARY BLACK HOLE MERGER GW150914 (2016, background): “However, these models adopt the optimistic assumption that in such mergers, even for grazing collisions, all of the mass is retained, leading to significant BH mass growth(Mapelli & Zampieri 2014; Ziosi et al. 2014).”
• The cosmic merger rate of neutron stars and black holes (2018, methodology): “…possibly large impact on the merger rate of compact objects (see e.g. Portegies Zwart & McMillan 2000; Mapelli et al. 2013; Mapelli & Zampieri 2014; Ziosi et al. 2014; Rodriguez et al. 2015, 2016; Mapelli 2016; Askar et al. 2017; Kimpson et al. 2016; Banerjee 2017; Zevin et al. 2017; Fujii et al.…”
• Massive black hole binaries from runaway collisions: the impact of metallicity (2016, methodology): “The reason is that metal-poor YDSCs host more massive BHs (which are more efficient in acquiring companions through dynamical interactions, Ziosi et al. 2014).”
• GW190521: Orbital Eccentricity and Signatures of Dynamical Formation in a Binary Black Hole Merger Signal (2020, background): “Young star clusters may create something of a hybrid channel, with dynamical interactions perturbing the evolution of primordial stellar binaries, which evolve to make merging double compact objects (Ziosi et al. 2014; Di Carlo et al. 2019; Rastello et al. 2020).”
• Binary Black Hole Population Properties Inferred from the First and Second Observing Runs of Advanced LIGO and Advanced Virgo (2018, background): “Meanwhile, BBH formation in dense stellar clusters(Ziosi et al. 2014; Rodriguez et al. 2015, 2016a; Mapelli 2016; Askar et al. 2017; Banerjee 2017) is impacted primarily by dynamical interactions within the cluster(Fregeau 2004; Morscher et al. 2013), but also by cluster size and initial mass…”
• Evolutionary roads leading to low effective spins, high black hole masses, and O1/O2 rates for LIGO/Virgo binary black holes (2017, background): “There may be yet another dynamical contribution from young open clusters to BHBH formations (Ziosi et al. 2014; Di Carlo et al. 2019).”
• Modeling Dense Star Clusters in the Milky Way and Beyond with the CMC Cluster Catalog (2019, background): “Furthermore, in this study we have considered only GCs; however, previous analyses (e.g., Ziosi et al. 2014; Banerjee 2018; Di Carlo et al. 2019) have shown that lower-mass open clusters may also contribute to the BBH merger rate.”
• Formation and Evolution of Compact-object Binaries in AGN Disks (2019, background): “…et al. 2019; Rastello et al. 2019) and dense star clusters (e.g., Portegies Zwart & McMillan 2000; O’Leary et al. 2006, 2016; Samsing et al. 2014; Ziosi et al. 2014; Mapelli 2016; Rodriguez et al. 2016a, 2016b; Askar et al. 2017; Fujii et al. 2017; di Carlo et al. 2019; Zevin et al. 2019;…”
• 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).”
• The progenitors of compact-object binaries: impact of metallicity, common envelope and natal kicks (2018, background): “…1995; Phinney 1996; Colpi et al. 2003; Mapelli et al. 2005; Grindlay et al. 2006; Ivanova et al. 2008; Clausen et al. 2013; Mapelli & Zampieri 2014; Ziosi et al. 2014; Rodriguez et al. 2015, 2016; Mapelli 2016; Askar et al. 2016; Antonini et al. 2017; Petrovich & Antonini 2017; Banerjee 2017;…”
• ILLUMINATING BLACK HOLE BINARY FORMATION CHANNELS WITH SPINS IN ADVANCED LIGO (2016, background): “…Mandel & De Mink 2016; Marchant et al. 2016), or the “dynamical” channel, in which BBHs are created though three-body encounters in dense star clusters (e.g., Sigurdsson & Hernquist 1993; Portegies Zwart & Mcmillan 2000; Downing et al. 2010, 2011; Ziosi et al. 2014; Rodriguez et al. 2015, 2016a).”
• Merging black hole binaries: the effects of progenitor's metallicity, mass-loss rate and Eddington factor (2017, background): “The impact of stellar dynamics on the formation of BHBs is also matter of debate (e.g. Ziosi et al. 2014; Rodriguez et al. 2015, 2016; Mapelli 2016; Askar et al. 2016; Antonini et al. 2017; Banerjee 2017).”
• The mass spectrum of compact remnants from the parsec stellar evolution tracks (2015, unknown): “…X-raybinaries(e.g. Blechaetal.2006;Mapellietal.2013;Mapelli &Zampieri2014),aswellastheformationandmergerofdouble-compact object binaries (e.g. O’Leary et al. 2006; Sadowski et al. 2008; Downing et al. 2010, 2011; Ziosi et al. 2014).”
• Merging black holes in young star clusters (2019, background): “…et al. 2003; O’Leary et al. 2006; Sadowski et al. 2008; O’Leary et al. 2009; Downing et al. 2010, 2011; Mapelli et al. 2013; 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;…”