MOCCA code for star cluster simulations – IV. A new scenario for intermediate mass black hole formation in globular clusters
By M. Giersz, N. Leigh, A. Hypki, N. Lützgendorf, A. Askar. 2015
188 citations recorded by the source corpus.
We discuss a new scenario for the formation of intermediate mass black holes (IMBHs) in dense star clusters. In this scenario, IMBHs are formed as a result of dynamical interactions of hard binaries containing a stellar-mass black hole (BH), with other stars and binaries. We discuss the necessary conditions to initiate the process of intermediate mass BH formation and the influence of an IMBH on the host global globular cluster (GC) properties. We discuss two scenarios for IMBH formation. The SLOW and FAST scenarios. They occur later or earlier in the cluster evolution and require smaller or extremely large central densities, respectively. In our simulations, the formation of IMBHs is highly stochastic. In general, higher formation probabilities follow from larger cluster concentrations (i.e. central densities). We further discuss possible observational signatures of the presence of IMBHs in GCs that follow from our simulations. These include the spatial and kinematic structure of the host cluster, possible radio, X-ray and gravitational wave emissions due to dynamical collisions or mass transfer and the creation of hypervelocity main-sequence escapers during strong dynamical interactions between binaries and an IMBH. All simulations discussed in this paper were performed with the MOCCA (MOnte Carlo Cluster simulAtor) Monte Carlo code. MOCCA accurately follows most of the important physical processes that occur during the dynamical evolution of star clusters but, as with other dynamical codes, it approximates the dissipative processes connected with stellar collisions and binary mergers.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/03f0d7e8fd9b09003a7fb03890d61db97ae3f781
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In Astronomy and Astrophysics
Citations in the corpus
- Massive black hole binaries from runaway collisions: the impact of metallicity (2016, background): “7 of Giersz et al. 2015).”
- Merging black hole binaries with the SEVN code (2018, background): “Stellar dynamics in dense star clusters can also affect the final mass of merging BHs (e.g. Portegies Zwart et al. 2004; Giersz et al. 2015; Mapelli 2016).”
- Merging black holes in young star clusters (2019, background): “Dynamical interactions in dense environments are also expected to significantly affect the mass spectrum of BHs (e.g. Portegies Zwart & McMillan 2000, 2002; Portegies Zwart et al. 2004; Gürkan et al. 2006; Giersz et al. 2015; Mapelli 2016).”
- MOCCA-SURVEY Database - I. Coalescing binary black holes originating from globular clusters (2016, background): “This was done to exclude merger events involving intermediate-mass black holes (IMBH) (Giersz et al. 2015).”
- N-body modelling of globular clusters: masses, mass-to-light ratios and intermediate-mass black holes (2016, background): “The high stellar densities in globular cluster could also give rise to the creation of intermediate-mass black holes (Portegies Zwart & McMillan 2002; Portegies Zwart et al. 2004; Giersz et al. 2015), which might be the progenitors of supermassive black holes in Galactic centers.”
- Very massive stars, pair-instability supernovae and intermediate-mass black holes with the sevn code (2017, background): “Furthermore, VMSs have also been claimed to be the progenitors of IMBHs (Portegies Zwart & McMillan 2002; Portegies Zwart et al. 2004; Freitag et al. 2006), but mass loss by stellar winds seems to be a key ingredient to understand their fate (Giersz et al. 2015; Mapelli 2016).”
- Black hole growth through hierarchical black hole mergers in dense star clusters: implications for gravitational wave detections (2018, background): “…whether intermediate mass BHs (IMBHs; generally defined as BHs with mass in the range ∼ 100 − 105M⊙) can form in globular clusters via hierarchical mergers of stellar seed BHs (e.g., Miller & Hamilton 2002c; Gültekin et al. 2004; Giersz et al. 2015; Kovetz et al. 2018; Christian et al. 2018).”
- Modeling Dense Star Clusters in the Milky Way and Beyond with the CMC Cluster Catalog (2019, background): “…conditions are met (i.e., if a cluster is sufficiently dense at early times), stellar collisions may lead to a runaway scenario, resulting in the formation of a very massive star and, ultimately, an IMBH (e.g., Portegies Zwart et al. 2004; Freitag et al. 2006; Giersz et al. 2015; Mapelli 2016).”
- The dragon simulations: globular cluster evolution with a million stars (2016, methodology): “…with semianalytical models (e.g. Alexander et al. 2014; Pijloo et al. 2015) and Monte-Carlo models have been presented (e.g. Joshi, Rasio, & Portegies Zwart 2000; Heggie & Giersz 2008; Giersz & Heggie 2011; Leigh et al. 2013, 2015; Chatterjee et al. 2013; Morscher et al. 2015; Giersz et al. 2015).”
- The cosmic merger rate of stellar black hole binaries from the Illustris simulation (2017, background): “Very massive BHs or even intermediate-mass BHs might form from runaway collisions (Portegies Zwart et al. 2004; Giersz et al. 2015; Mapelli 2016).”