2025/03/01 by S. V. Pilipenko, С. В. Пилипенко, M. V. Tkachev +1 · 1 citation
Physics and Astronomy · #Astronomy #Astrophysics #Black Holes and Theoretical Physics #Cosmology and Gravitation Theories #Dwarf galaxy #Galaxies: Formation, Evolution, Phenomena #Galaxy #Halo #Physics #Primordial black hole #Spin-flip
paper · pdf · doi:10.1134/s0021364024604664
published in Journal of Experimental and Theoretical Physics Letters 121(5), 324-331 (Pleiades Publishing)
openalex publication_date 2025/03/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/25
Through numerical experiments, we have predicted that if dark matter contains even a small fraction, f0 ∼ 10^ - 4 , of primordial black holes (PBHs), during the formation of the gravitationally bound halo of a dwarf galaxy, these PBHs will concentrate in a region with a radius of about 10 pc, so that their local fraction will exceed 1%. Unlike previous studies of PBH migration to the centers of galaxies, the numerical experiments conducted here take into account the early formation of a massive “dress” of dark matter around the PBHs and the non-stationarity of the halo during its formation. Applying our results to models of heating stellar clusters in the Eridanus II and Segue I galaxies due to dynamical friction between stars and PBHs allows us to impose constraints on the abundance of PBHs that are two orders of magnitude stricter than previously thought.