Compact binaries in star clusters – I. Black hole binaries inside globular clusters

By J. Downing, M. Benacquista, M. Giersz, Rainer Spurzem. 2009

150 citations recorded by the source corpus.

We study the compact binary population in star clusters, focusing on binaries containing black holes, using a self-consistent Monte Carlo treatment of dynamics and full stellar evolution. We find that the black holes experience strong mass segregation and become centrally concentrated. In the core the black holes interact strongly with each other and black hole–black hole binaries are formed very efficiently. The strong interactions, however, also destroy or eject the black hole–black hole binaries. We find no black hole–black hole mergers within our simulations but produce many hard escapers that will merge in the Galactic field within a Hubble time. We also find several highly eccentric black hole–black hole binaries that are potential Laser Interferometer Space Antenna (LISA) sources, suggesting that star clusters are interesting targets for space-based detectors. We conclude that star clusters must be taken into account when predicting compact binary population statistics.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/3222bf1da205ed9b4ca8841d631888f78ebf1e4f

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In Astronomy and Astrophysics

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

Citations in the corpus

• 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).”
• Stellar-mass black holes in young massive and open stellar clusters and their role in gravitational-wave generation (2016, background): “…recent direct N-body (e.g., Banerjee et al. 2010; Aarseth 2012; Sippel & Hurley 2013; Wang et al. 2016; Hurley et al. 2016) and Monte-Carlo (e.g., Downing et al. 2010, 2011; Rodriguez et al. 2015; Morscher et al. 2015; Rodriguez et al. 2016a,b; Chatterjee et al. 2016a,b; Askar et al. 2016)…”
• 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).”
• Black hole growth through hierarchical black hole mergers in dense star clusters: implications for gravitational wave detections (2018, methodology): “Numerical simulations 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,…”
• Binary Black Hole Population Properties Inferred from the First and Second Observing Runs of Advanced LIGO and Advanced Virgo (2018, background): “…Sigurdsson & Hernquist 1993; Portegies Zwart & McMillan 2000; Grindlay et al. 2006; O’Leary et al. 2006; Ivanova et al. 2008; Sadowski et al. 2008; Downing et al. 2010, 2011; Clausen et al. 2013; Ziosi et al. 2014; Rodriguez et al. 2015, 2016a; Mapelli 2016; Askar et al. 2017; Banerjee 2017;…”
• Evolutionary roads leading to low effective spins, high black hole masses, and O1/O2 rates for LIGO/Virgo binary black holes (2017, background): “…open, young clusters (Miller & Hamilton 2002a,b; Portegies Zwart et al. 2004; Gültekin et al. 2004, 2006; O’Leary et al. 2007; Sadowski et al. 2008; Downing et al. 2010; Benacquista & Downing 2013; Bae et al. 2014; Chatterjee et al. 2017; Mapelli 2016; Hurley et al. 2016; Rodriguez et al. 2016a;…”
• 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).”
• DOUBLE COMPACT OBJECTS. III. GRAVITATIONAL-WAVE DETECTION RATES (2015, unknown): “…in which dynamical interactions between stars are important (i.e., globular clusters and galactic nuclear clusters) have been presented elsewhere (Gültekin et al. 2004; Grindlay et al. 2006; O’Leary et al. 2006; Ivanova et al. 2008; Sadowski et al. 2008; Miller & Lauburg 2009; Downing et al. 2010).”
• Massive black hole binaries from runaway collisions: the impact of metallicity (2016, background): “…find that most BH-BH mergers in YDSCs are expected to occur between low-mass BHs (5 − 15 M⊙), despite the efficiency of dynamical exchanges (see also Downing et al. 2010, 2011; O’Leary et al. 2006; Sadowski et al. 2008; Clausen et al. 2013; Morscher et al. 2015; Rodriguez et al. 2015;…”
• Dynamical evolution of black hole subsystems in idealized star clusters (2013, unknown): “G A ] 1 1 A pr 2 (1993), Portegies Zwart & McMillan (2000), Banerjee et al (2010), Downing et al (2010), Aarseth (2012)).”
• Merging black holes in young star clusters (2019, background): “…1993; Sigurdsson & Phinney 1995; Portegies Zwart & McMillan 2000; Colpi 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;…”
• Dynamics of stellar black holes in young star clusters with different metallicities – II. Black hole–black hole binaries (2014, methodology): “On the other hand, our simulated star clusters are a factor of 10−1000 less massive and a factor of ≥5 smaller than those studied in previous work (e.g. Downing et al. 2010).”
• ASTROPHYSICAL IMPLICATIONS OF THE BINARY BLACK HOLE MERGER GW150914 (2016, methodology): “The first simulations to account in detail for both binary evolution and stellar dynamics with a BH mass spectrum and with realistic numbers of particles were by Downing et al. (2010, 2011) and by Morscher et al. (2013, 2015).”
• BLACK HOLE MERGERS AND BLUE STRAGGLERS FROM HIERARCHICAL TRIPLES FORMED IN GLOBULAR CLUSTERS (2015, background): “This latter value for the chirp mass is the maximum for primordial binaries in our GC simulations that evolved without significant dynamical encounters (see also Downing et al. 2010; Rodriguez et al. 2015).”
• Constraining Formation Models of Binary Black Holes with Gravitational-wave Observations (2017, background): “…that become bound and tighten through three-body encounters in dense star clusters such as globular clusters (e.g., Portegies Zwart & McMillan 2000; Downing et al. 2010, 2011; Rodriguez et al. 2016a, 2015), galactic nuclei and AGN disks (Antonini & Rasio 2016; Bartos et al. 2017; Stone et al.…”
• DOUBLE COMPACT OBJECTS. I. THE SIGNIFICANCE OF THE COMMON ENVELOPE ON MERGER RATES (2012, background): “…dense pop- ulations in which dynamical interactions between stars are important (i.e., globular clusters) have been presented elsewhere (Gültekin et al., 2004; O’Leary et al., 2006; Grindlay et al., 2006; Sadowski et al., 2008; Ivanova et al., 2008; Downing et al., 2010; Miller & Lauburg, 2009).”