Exact solutions and cosmological constraints in fractional cosmology

Abstract

This paper investigates exact solutions of cosmological interest in fractional cosmology. Given $\mu$, the order of Caputo's fractional derivative, and $w$, the matter equation of state, we present specific exact power-law solutions. We discuss the exact general solution of the Riccati Equation, where the solution for the scale factor is a combination of power laws. Using cosmological data, we estimate the free parameters. An analysis of type Ia supernovae (SNe Ia) data and the observational Hubble parameter data (OHD), also known as cosmic chronometers, and a joint analysis with data from SNe Ia + OHD leads to best-fit values for the free parameters calculated at $1\sigma$, $2\sigma$ and $3\sigma$ confidence levels (CLs). On the other hand, these best-fit values are used to calculate the age of the Universe, the current deceleration parameter (both at $3\sigma$ CL) and the current matter density parameter at $1\sigma$ CL. Finding a Universe roughly twice as old as the one of $\Lambda$CDM is a distinction of fractional cosmology. Focusing our analysis on these results, we can conclude that the region in which $\mu >2$ is not ruled out by observations. This parameter region is relevant because fractional cosmology gives a power-law solution without matter, which is accelerated for $\mu >2$. We present a fractional origin model that leads to an accelerated state without appealing to $\Lambda$ or dark energy.

56 pages, 10 figures. This article belongs to the Special Issue Fractional Gravity/Cosmology in Classical and Quantum Regimes in Fractal and Fractional

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• Conformal and Non-Minimal Couplings in Fractional Cosmology
• Fractional Einstein-Gauss-Bonnet scalar field cosmology
• Fractional Einstein field equations in $2+1$ dimensional spacetime
• Fractional entropy of the Brown-Kuchař dust in fractional anti-de Sitter quantum gravity
• Inflation and Primordial Perturbations in Fractal Cosmology
• Emergent $\Lambda$CDM cosmology from a measure-induced deformation of the Newtonian action