Any unified early and late dark energy scenario with a single tracking scalar field requires a potential with three distinct slopes arranged in a steep-steeper-shallow hierarchy.
On the interacting dark en- ergy scenarios−the case for Hubble constant tension,
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N-body simulations of IDE with Q=ξHρ_x show scale-dependent deviations in the matter power spectrum, density morphology, and halo abundance that standard ΛCDM-calibrated prescriptions cannot reproduce.
Gravitationally induced particle creation models fit cosmological data as well as ΛCDM and reduce the Hubble tension from 4.3σ to 2.4–3σ.
Generalizes the interacting dilatonic ghost condensate dark energy model, performs phase-space analysis for non-interacting and two interacting cases, and reports parameter constraints from Cosmic Chronometers, PantheonPlus, and DESI data for n=3 and n=5.
citing papers explorer
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Unifying Early and Late Dark Energy: Dynamical Requirements and Obstructions
Any unified early and late dark energy scenario with a single tracking scalar field requires a potential with three distinct slopes arranged in a steep-steeper-shallow hierarchy.
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Non-linear Structure Formation in Planck+DESI Favoured Interacting Dark Energy Cosmologies
N-body simulations of IDE with Q=ξHρ_x show scale-dependent deviations in the matter power spectrum, density morphology, and halo abundance that standard ΛCDM-calibrated prescriptions cannot reproduce.
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Revisiting the Matter Creation Process: Observational Constraints on Gravitationally Induced Dark Energy and the Hubble Tension
Gravitationally induced particle creation models fit cosmological data as well as ΛCDM and reduce the Hubble tension from 4.3σ to 2.4–3σ.
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Generalizing the interacting dilatonic ghost condensate as a dark energy model
Generalizes the interacting dilatonic ghost condensate dark energy model, performs phase-space analysis for non-interacting and two interacting cases, and reports parameter constraints from Cosmic Chronometers, PantheonPlus, and DESI data for n=3 and n=5.