Inhomogenous Chaotic Inflation

TL;DR

This paper proposes a chaotic inflation model driven by a classical scalar field, leading to an inhomogeneous early universe that evolves into a homogeneous, isotropic universe, without relying on Planck-scale physics.

Contribution

It introduces a singularity-free chaotic inflation model with inhomogeneous initial conditions that naturally evolve into a standard cosmological history.

Findings

Inhomogeneous inflation can produce a low-temperature universe.

The model accounts for baryogenesis and subsequent standard cosmological phases.

It does not depend on Planck-scale physics.

Abstract

A chaotic model of the early universe within the framework of the singularity-free solutions of Einstein's equation is suggested. The evolution of our universe at its early stage, starting out as a small domain of the parent universe, is governed by the dynamics of a classical scalar field $\phi$ . If in any such domain, larger than Planck length,$\dot \phi$ happens to be very large,$\phi$ may develop a dominant inhomogeneous mode,leading to an anisotropic inflation of the universe. The particle $\phi$ is coupled to other particles, which are produced copiously after inflation and these thermalize leading to a rather low temperature universe $(T \geq 10^{4} $ Gev). The electroweak B+L Baryogenesis is assumed to account for the observed baryon asymmetry. The universe now passes through a radiation-dominated phase, leading eventually to a matter-dominated universe, which is isotropic and homogeneous. The model does not depend on the details of Planck scale physics.