Properties of the exact analytic solution of the growth factor and its applications

Abstract

There have been the approximate analytic solution \cite{Silveria} and several approximate analytic forms \cite{0508156,Carroll,0303112} of the growth factor $D_g$ for the general dark energy models with the constant values of its equation of state $\omde$ after Heath found the exact integral form of the solution of $D_g$ for the Universe including the cosmological constant or the curvature term. Recently, we obtained the exact analytic solutions of the growth factor for both $\omde = -1$ or $-\fr{1}{3}$ \cite{SK1} and the general dark energy models with the constant equation of state $\omde$ \cite{SK3} independently. We compare the exact analytic solution of $D_g$ with the other well known approximate solutions. We also prove that the analytic solutions for $\omde = -1$ or $-\fr{1}{3}$ in Ref. \cite{SK1} are the specific solutions of the exact solutions of the growth factor for general $\omde$ models in Ref. \cite{SK3} even though they look quite different. We scrutinize the issue of using the well known parameterizations of the growth index and its parameter given in Ref. \cite{WS} to obtain the growth factor for general dark energy models. We also investigate the possible extensions of the exact solution of $D_g$ to the time-varying $\omde$ for the comparison with observations.

18 pages, 10 figures, 3 tables, To match the version accepted by Physical Review D

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• Modified Gravity and Cosmology
• Spherical collapse model with non-clustering dark energy
• Growth index with the exact analytic solution of sub-horizon scale linear perturbation for dark energy models with constant equation of state
• Growth Rate in the Dynamical Dark Energy Models
• Spherical collapse model with and without curvature
• Constraints on scalar-tensor theories of gravity from observations
• Measuring the matter energy density and Hubble parameter from Large Scale Structure
• Lagrangian perturbations theory : Third-order solution for general dark energy models
• Cluster number counts in quintessence models
• Probing Time-Varying Dark Energy with DESI: The Crucial Role of Precision Matter Density (Ω_{m0}) Measurements
• Perspectives for studying the dark energy at z>2 with galaxy surveys