The Stability of an Isotropic Cosmological Singularity in Higher-Order Gravity

Details The Stability of an Isotropic Cosmological Singularity in Higher-Order Gravity The Stability of an Isotropic Cosmological Singularity in Higher-Order Gravity

2008-01-26

arxiv.org/abs/0801.4090v1

Phys.Rev.D77:103523,2008

Astronomy and Astrophysics

Astrophysics

General Relativity and Quantum Cosmology

25 pages

Scientific paper

10.1103/PhysRevD.77.103523

We study the stability of the isotropic vacuum Friedmann universe in gravity theories with higher-order curvature terms of the form $(R_{ab}R^{ab})^{n}$ added to the Einstein-Hilbert Lagrangian of general relativity on approach to an initial cosmological singularity. Earlier, we had shown that, when $% n=1$, a special isotropic vacuum solution exists which behaves like the radiation-dominated Friedmann universe and is stable to anisotropic and small inhomogeneous perturbations of scalar, vector and tensor type. This is completely different to the situation that holds in general relativity, where an isotropic initial cosmological singularity is unstable in vacuum and under a wide range of non-vacuum conditions. We show that when $n\neq 1$, although a special isotropic vacuum solution found by Clifton and Barrow always exists, it is no longer stable when the initial singularity is approached. We find the particular stability conditions under the influence of tensor, vector, and scalar perturbations for general $n$ for both solution branches. On approach to the initial singularity, the isotropic vacuum solution with scale factor $a(t)=t^{P_{-}/3}$ is found to be stable to tensor perturbations for $0.51$ and is unstable as $t \to 0$ for all $n$ for each type of perturbation.

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