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Primordial Black Hole clusters, phenomenology & implications
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abstract
We present direct N-body simulations of black-hole-only clusters with up to $2 \cdot 10^4$ compact objects, zero natal spin and no primordial binaries as predicted by various primordial black hole (PBH) Dark Matter models. The clusters' evolution is computed using ${\tt NBODY6\!+\!+GPU}$, including the effects of the tidal field of the galaxy, the kicks of black hole mergers and orbit-averaged energy loss by gravitational radiation of binaries. We investigate clusters with four initial mass distributions, three of which attempt to model a generic PBH scenario using a lognormal mass distribution and a fourth one that can be directly linked to a monochromatic PBH scenario when accretion is considered. More specifically, we dive into the clusters' internal dynamics, describing their expansion and evaporation, along with the resultant binary black hole mergers. We also compare several simulations with and without black hole merger kicks and find modelling implications for the probability of hierarchical mergers.
Forward citations
Cited by 4 Pith papers
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Evolution of a black hole cluster in full general relativity
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Harvesting primordial black holes from stochastic trees with $\texttt{FOREST}$
A stochastic-branching-tree implementation of inflation, FOREST, computes curvature maps and primordial black hole mass functions with cloud-in-cloud effects included.
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Do Primordial Black Hole Clusters Survive the Galaxy? Collisional Disruption and Microlensing Implications
Cluster-cluster collisions strip 50–96% of 10^6–10^7 M⊙ PBH cluster mass by z=0, so microlensing sightlines to the Magellanic Clouds are ~49–92% smooth.
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Spin-up and mass-gain in hyperbolic encounters of spinning black holes
Scattering black holes gain spin and mass by absorbing emitted gravitational radiation, with spin-up up to 0.3 and mass gain up to 15% in near-threshold encounters.
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