Instability of scalar perturbation in a phantomic cosmological scenario

Abstract

Scalar perturbations can grow during a phantomic cosmological phase as the big rip is approached, in spite of the high accelerated expansion regime, if the equation of state is such that $\frac{p}{\rho }=\alpha <-5/3$. It is shown that such result is independent of the spatial curvature. The perturbed equations are exactly solved for any value of the curvature parameter $k$ and of the equation of state parameter $\alpha$. Growing modes are found asymptotically under the condition $\alpha <-5/3$. Since the Hubble radius decreases in a phantom universe, such result indicates that a phantom scenario may not survive longtime due to gravitational instability.

arXiv commentLatex file, 6 pages

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Cited by in corpus (3)

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• Some remarks on the observational constraints on the self-interacting scalar field model for dark energy