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SUMMARY:Dynamical evolution of primordial black hole clusters with lognorm
 al mass distribution
DTSTART;VALUE=DATE-TIME:20261029T064500Z
DTEND;VALUE=DATE-TIME:20261029T070000Z
DTSTAMP;VALUE=DATE-TIME:20261024T220022Z
UID:indico-contribution-6248@cern.ch
DESCRIPTION:Speakers: Yana Savchenko (Novosibirsk State University\, Budke
 r Institute of Nuclear Physics)\nBlack holes formed in the early Universe 
 (primordial black holes\, PBHs) may simultaneously explain several astroph
 ysical anomalies. These include\, for example\, the existence of supermass
 ive black holes in the young Universe ($z>6$\, [Mazzucchelli C. et al.\, (
 2017\, ApJ)][1]) and black holes with masses of $\\sim30 M_\\odot$ detecte
 d by gravitational-wave observatories ([LVK Scientific Collaboration et al
 . 2025][2]) that fall into the “forbidden” mass gap for remnants of st
 ellar collapse [(Abbott R. et al. (2020b\, Phys. Rev. Lett.))][3]. PBHs ma
 y also contribute a fraction of the dark matter (DM)\, although for solar 
 mass range it is already constrained by $\\leq 10\\%$  [(P. Mroz et al. (2
 024\, Nature))][4].\n\nIn the basic scenario\, it is assumed that PBHs are
  spatially uncorrelated. However\, if PBHs are derived from large non-Gaus
 sian tails of density contrast\, they can be spatially clustered at birth 
 ([Animali et al.\, (2024\, JCAP)][5]). There are other models that lead to
  clustering such as the modified Affleck-Dine mechanism ([Kawasaki et al.\
 , (2021\, JCAP)][6]). The clustering of PBHs would change the merger histo
 ry of PBHs\, therefore it is important to study such systems.\n\nWe presen
 t a numerical study of dynamical evolution of isolated primordial black ho
 le clusters. We use mass distribution of PBHs derived from LIGO-Virgo-Kagr
 a data fit ([Dolgov et al.\, (2020\, JCAP)][7]\; [Andres-Carcasona et al. 
 (2024\, Phys. Rev. D.)][8]). The evolution of clusters was computed using 
 the direct N-body code $\\textbf{NBODY6++GPU}$ and takes into account orbi
 t-averaged gravitational wave emission. We explore how the parameters of s
 uch clusters affect the merger rate and masses of merging binaries.\n\n\n 
  [1]: https://ui.adsabs.harvard.edu/link_gateway/2017ApJ...849...91M/doi:1
 0.3847/1538-4357/aa9185\n  [2]: https://ui.adsabs.harvard.edu/link_gateway
 /2025arXiv250818082T/doi:10.48550/arXiv.2508.18082\n  [3]: https://doi.org
 /10.1103/PhysRevLett.125.101102\n  [4]: https://ui.adsabs.harvard.edu/link
 _gateway/2024Natur.632..749M/doi:10.1038/s41586-024-07704-6\n  [5]: https:
 //doi.org/10.48550/arXiv.2402.08642\n  [6]: https://doi.org/10.48550/arXiv
 .2107.03580\n  [7]: https://doi.org/10.1088/1475-7516/2020/12/017\n  [8]: 
 https://doi.org/10.1103/PhysRevD.110.023040\n\nhttps://indico.particle.mep
 hi.ru/event/626/contributions/6248/
LOCATION:Sevastopol Hotel
URL:https://indico.particle.mephi.ru/event/626/contributions/6248/
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