Bubbles kick off primordial black holes to form more binaries
Primordial black holes (PBHs) may form before cosmological first-order phase transitions, leading to inevitable collisions between PBHs and bubble walls. In this paper, we have simulated the coevolution of an expanding scalar wall passing through a black
Zi-Yan Yuwen +3 more
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Structure of the Baryon Halo Around a Supermassive Primordial Black Hole
According to some theoretical models, primordial black holes with masses of more than 108 solar masses could be born in the early universe, and their possible observational manifestations have been investigated in a number of works. Dense dark matter and
Boris Murygin +2 more
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Dark spiky primordial black holes
11 pages, 1 figure; matches published ...
openaire +2 more sources
Primordial black holes and scalar-induced gravitational waves from the perturbations on the inflaton potential in peak theory [PDF]
Ji-Xiang Zhao, Xiaohui Liu, Nan Li
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Nonlinear metric perturbations and production of primordial black holes [PDF]
P. B. Ivanov
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Large fluctuations and primordial black holes
In this paper, we review in detail different mechanisms of generation of large primordial fluctuations and their implications for the production of primordial black holes (PBHs) and scalar-induced secondary gravity waves (SIGW), with the ultimate aim of understanding the impact of loop correction on quantum correlations and the power spectrum.
Choudhury, Sayantan, Sami, M.
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Probing Primordial Black Holes with Angular Power Spectrum for Anisotropies in Stochastic Gravitational-Wave Background [PDF]
Sai Wang, Kazunori Kohri
openalex
NANOGrav Results and LIGO-Virgo Primordial Black Holes in Axionlike Curvaton Models [PDF]
Keisuke Inomata +3 more
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87th Annual Meeting of the Meteoritical Society 2025: Abstracts
Meteoritics &Planetary Science, Volume 60, Issue S1, Page 30-350, August 2025.
wiley +1 more source
How open is the asteroid-mass primordial black hole window?
Primordial black holes (PBHs) can make up all of the dark matter (DM) if their mass, $m$, is in the so-called "asteroid-mass window", $10^{17} g ≲ m ≲ 10^{22} g$. Observational constraints on the abundance of PBHs are usually calculated assuming they all
Matthew Gorton, Anne M. Green
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