Analytic Solutions of Scalar Field Cosmology, Mathematical Structures for Early Inflation and Late Time Accelerated Expansion

TL;DR

This paper derives analytical solutions for scalar field cosmology models, providing insights into early inflation and late-time acceleration, and explores the role of domain walls in cosmic expansion.

Contribution

It introduces a method to analytically solve scalar field cosmology equations with a change of variables, linking mathematical solutions to cosmic acceleration phenomena.

Findings

Mathematically solvable models for scalar field cosmology.

Late-time acceleration explained by cosmic domain walls.

Potential to resolve Hubble tension with domain wall dominance.

Abstract

We study the most general cosmological model with real scalar field which is minimally coupled to gravity. Our calculations are based on Friedmann-Lemaitre-Robertson-Walker (FLRW) background metric. Field equations consist of three differential equations. We switch independent variable from time to scale factor by change of variable $\dot{a}/a=H(a)$. Thus a new set of differential equations are analytically solvable with known methods. We formulate Hubble function, the scalar field, potential and energy density when one of them is given in the most general form. $a(t)$ can be explicitly found as long as methods of integration techniques are available. We investigate the dynamics of the universe at early times as well as at late times in light of these formulas. We find mathematical machinery which turns on and turns off early accelerated expansion. On the other hand late time accelerated expansion is explained by cosmic domain walls. We have compared our results with recent observations of type Ia supernovae by considering the Hubble tension and absolute magnitude tension. Eighty-nine percent of present universe may consist of domain walls while rest is matter.