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On the Increase in the Density of Primordial Black Holes in the Halos of Dwarf Galaxies
被引：0
作者：
S. V. Pilipenko
[1
]
M. V. Tkachev
[1
]
N. R. Arakelyan
[1
]
机构：
[1] Astro Space Center,
[2] Lebedev Physical Institute,undefined
[3] Russian Academy of Sciences,undefined
关键词：
D O I：
10.1134/S0021364024604664
中图分类号：
学科分类号：
摘要：
Through numerical experiments, we have predicted that if dark matter contains even a small fraction, \documentclass[12pt]{minimal}
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\begin{document}$${{f}_{0}} \sim {{10}^{{ - 4}}}$$\end{document}, 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.
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页码：324 / 331
页数：7
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