Little Ado about Everything: \(\eta\)CDM, a Cosmological Model with Fluctuation-driven Acceleration at Late Times

• Published in: arXiv.org
• Main Authors: Lapi, Andrea, Boco, Lumen, Cueli, Marcos M, Haridasu, Balakrishna S, Ronconi, Tommaso, Baccigalupi, Carlo, Danese, Luigi
• Format: Paper
• Language: English
• Published: Ithaca Cornell University Library, arXiv.org 27.10.2023
• Subjects: Astronomical models; Cosmology; Dark energy; Evolution; Homogeneity; Isotropy; Parameterization; Spatial distribution; Universe
• ISSN: 2331-8422

[abridged] We propose a model of the Universe (dubbed \(\eta\)CDM) featuring a stochastic evolution of the cosmological quantities, that is meant to render small deviations from homogeneity/isotropy on scales of \(30-50\, h^{-1}\) Mpc at late cosmic times, associated to the emergence of the cosmic web. Specifically, we prescribe that the behavior of the matter/radiation energy densities in different patches of the Universe with such a size can be effectively described by a stochastic version of the mass-energy evolution equation. The latter includes an appropriate noise term that statistically accounts for local fluctuations due to inhomogeneities, anisotropic stresses and matter flows. The evolution of the different patches as a function of cosmic time is rendered via the diverse realizations of the noise term; meanwhile, at any given cosmic time, sampling the ensemble of patches will originate a nontrivial spatial distribution of the cosmological quantities. The overall behavior of the Universe will be obtained by averaging over the patch ensemble. We assume a physically reasonable parameterization of the noise term, gauging it against a wealth of cosmological datasets. We find that, with respect to standard \(\Lambda\)CDM, the ensemble-averaged cosmic dynamics in the \(\eta\)CDM model is substantially altered in three main respects: (i) an accelerated expansion is enforced at late cosmic times without the need for any additional exotic component (e.g., dark energy); (ii) the spatial curvature can stay small even in a low-density Universe; (iii) matter can acquire an effective negative pressure at late times. We provide predictions for the variance of the cosmological quantities among different patches of the Universe at late cosmic times. Finally, we show that in \(\eta\)CDM the Hubble-tension is solved, and the cosmic coincidence problem is relieved without invoking the anthropic principle.