Primordial black holes as cosmic expansion accelerators

We propose a novel and natural mechanism for cosmic acceleration driven by primordial black holes (PBHs) exhibiting repulsive behavior. Using a new ``Swiss Cheese’’ cosmological approach, we demonstrate that this cosmic acceleration mechanism is a general phenomenon by examining three regular black hole spacetimes - namely the Hayward, the Bardeen and the Dymnikova spacetimes - as well as the singular de Sitter-Schwarzschild spacetime. Interestingly, by matching these black hole spacetimes with an isotropic and homogeneous expanding Universe, we obtain a phase of cosmic acceleration that ends at an energy scale characteristic to the black hole parameters or due to black hole evaporation. This cosmic acceleration mechanism can be relevant either to an inflationary phase with a graceful exit and reheating or to an early dark energy type of contribution pertinent to the Hubble tension. Remarkably, we find that ultra-light PBHs with masses $m<5\times 10^8\mathrm{g}$ dominating the energy content of the Univese before Big Bang Nucleosynthesis, can drive a successful inflationary expansion era without the use of an inflaton field. Additionally, PBHs with masses $m \sim 10^{12}\mathrm{g}$ and abundances $0.107 < Ω^\mathrm{eq}_\mathrm{PBH}< 0.5$, slightly before matter-radiation equality, can produce a substantial amount of early dark energy, helping to alleviate the $H_0$ tension.

💡 Research Summary

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The paper proposes that primordial black holes (PBHs) with a repulsive core can act as natural drivers of cosmic acceleration when embedded in an expanding Friedmann‑Lemaître‑Robertson‑Walker (FLRW) background via a “Swiss‑Cheese” construction. The authors examine four spacetimes: three regular black‑hole solutions (Hayward, Bardeen, Dymnikova) characterized by a regularisation scale L, and the singular de Sitter–Schwarzschild metric, which is repulsive at large radii. By matching a spherical black‑hole region to the FLRW exterior using standard junction conditions, they derive modified Friedmann equations. The key result is

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