Inflation with stable anisotropic hair: is it cosmologically viable?

TL;DR

This paper investigates an inflationary model with anisotropic features, demonstrating its viability by analyzing its behavior in curved, anisotropic spacetimes and showing it can produce a universe consistent with observations.

Contribution

It extends previous work by including curvature and analyzing anisotropic inflation in Bianchi type II, III, and Kantowski-Sachs spacetimes, confirming the model's cosmological viability.

Findings

The anisotropic fix-point is an attractor for various spacetimes.

The universe approaches this fix-point after a few e-folds for many initial conditions.

Inflation with anisotropic hair can produce a universe consistent with observational isotropy.

Abstract

Recently an inflationary model with a vector field coupled to the inflaton was proposed and the phenomenology studied for the Bianchi type I spacetime. It was found that the model demonstrates a counter-example to the cosmic no-hair theorem since there exists a stable anisotropically inflationary fix-point. One of the great triumphs of inflation, however, is that it explains the observed flatness and isotropy of the universe today without requiring special initial conditions. Any acceptable model for inflation should thus explain these observations in a satisfactory way. To check whether the model meets this requirement, we introduce curvature to the background geometry and consider axisymmetric spacetimes of Bianchi type II,III and the Kantowski-Sachs metric. We show that the anisotropic Bianchi type I fix-point is an attractor for the entire family of such spacetimes. The model is predictive in the sense that the universe gets close to this fix-point after a few e-folds for a wide range of initial conditions. If inflation lasts for N e-folds, the curvature at the end of inflation is typically of order exp(-2N). The anisotropy in the expansion rate at the end of inflation, on the other hand, while being small on the one-percent level, is highly significant. We show that after the end of inflation there will be a period of isotropization lasting for about 2N/3 e-folds. After that the shear scales as the curvature and becomes dominant around N e-folds after the end of inflation. For plausible bounds on the reheat temperature the minimum number of e-folds during inflation, required for consistency with the isotropy of the supernova Ia data, lays in the interval (21,48). Thus the results obtained for our restricted class of spacetimes indicates that inflation with anisotropic hair is cosmologically viable.