Repulsive-like primordial black holes in the Swiss-cheese framework produce quasi-de Sitter expansion, enabling inflation with evaporation reheating and acting as early dark energy for certain masses and densities.
Structure formation with a self-tuning scalar field
4 Pith papers cite this work. Polarity classification is still indexing.
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abstract
A scalar field with an exponential potential has the particular property that it is attracted into a solution in which its energy scales as the dominant component (radiation or matter) of the Universe, contributing a fixed fraction of the total energy density. We study the growth of perturbations in a CDM dominated $\Omega=1$ universe with this extra field, with an initial flat spectrum of adiabatic fluctuations. The observational constraints from structure formation are satisfied as well, or better, than in other models, with a contribution to the energy density from the scalar field $\Omega_\phi \sim 0.1$ which is small enough to be consistent with entry into the attractor prior to nucleosynthesis.
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Replacing the cosmological constant with the Kretschmann scalar yields a dynamical dark energy model that fits supernova and cosmic chronometer data and produces a phantom-crossing equation-of-state parameter w(z) similar to recent phenomenological fits.
Cosmological data can constrain only a handful of EFT parameters for single-scalar dark energy; extended models show modest preference over Λ but remain underdetermined and challenged by fifth forces and screening.
In a 5D open FRW model, negative curvature sustains tracker-like radion evolution that enables dynamical compactification via Casimir stabilization before 4D inflation dilutes curvature remnants.
citing papers explorer
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Inflation driven by repulsive-like primordial black holes
Repulsive-like primordial black holes in the Swiss-cheese framework produce quasi-de Sitter expansion, enabling inflation with evaporation reheating and acting as early dark energy for certain masses and densities.
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Dynamical dark energy from Kretschmann scalar at low redshifts
Replacing the cosmological constant with the Kretschmann scalar yields a dynamical dark energy model that fits supernova and cosmic chronometer data and produces a phantom-crossing equation-of-state parameter w(z) similar to recent phenomenological fits.
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The Status of Single Scalar Field Dark Energy
Cosmological data can constrain only a handful of EFT parameters for single-scalar dark energy; extended models show modest preference over Λ but remain underdetermined and challenged by fifth forces and screening.
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Curvature-Assisted Dynamical Compactification in a Pre-Inflationary Higher-Dimensional Universe
In a 5D open FRW model, negative curvature sustains tracker-like radion evolution that enables dynamical compactification via Casimir stabilization before 4D inflation dilutes curvature remnants.