Effects of spatial curvature and anisotropy on the asymptotic regimes in Einstein-Gauss-Bonnet gravity

TL;DR

This paper investigates how spatial curvature and anisotropy influence the late-time behavior of Einstein-Gauss-Bonnet cosmologies, revealing conditions for stabilization and isotropization of extra dimensions.

Contribution

It provides a detailed analysis of the effects of curvature and anisotropy on asymptotic regimes, highlighting differences between cases with two and three or more extra dimensions.

Findings

Negative curvature stabilizes extra dimensions for D ≥ 3.

Transition from Kasner to exponential expansion is stable under anisotropy.

Isotropization occurs dynamically from general anisotropic initial conditions for D ≥ 3.

Abstract

In this paper we address two important issues which could affect reaching the exponential and Kasner asymptotes in Einstein-Gauss-Bonnet cosmologies -- spatial curvature and anisotropy in both three- and extra-dimensional subspaces. In the first part of the paper we consider cosmological evolution of spaces being the product of two isotropic and spatially curved subspaces. It is demonstrated that the dynamics in $D=2$ (the number of extra dimensions) and $D \geqslant 3$ is different. It was already known that for the $\Lambda$-term case there is a regime with "stabilization" of extra dimensions, where the expansion rate of the three-dimensional subspace as well as the scale factor (the "size") associated with extra dimensions reach constant value. This regime is achieved if the curvature of the extra dimensions is negative. We demonstrate that it take place only if the number of extra dimensions is $D \geqslant 3$. In the second part of the paper we study the influence of initial anisotropy. Our study reveals that the transition from Gauss-Bonnet Kasner regime to anisotropic exponential expansion (with expanding three and contracting extra dimensions) is stable with respect to breaking the symmetry within both three- and extra-dimensional subspaces. However, the details of the dynamics in $D=2$ and $D \geqslant 3$ are different. Combining the two described affects allows us to construct a scenario in $D \geqslant 3$, where isotropisation of outer and inner subspaces is reached dynamically from rather general anisotropic initial conditions.