Instability of scalar perturbation in a phantomic cosmological scenario

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dc.creatorFabris, J. C.
dc.creatorJardim, D. F.
dc.creatorGoncalves, S. V. B.
dc.date2007-12-03
dc.date.accessioned2026-07-07T11:54:30Z
dc.date.available2026-07-07T11:54:30Z
dc.descriptionScalar 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 $\frac{p}ρ = α< - {5/3}$. 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 $α$. Growing modes are found asymptotically under the condition $α< - {5/3}$. Since the Hubble radius decreases in a phantom universe, such result indicates that a phantom scenario may not survive longtime due to gravitational instability.
dc.descriptionLatex file, 6 pages
dc.identifierhttps://arxiv.org/abs/0712.0272
dc.identifierhttp://arxiv.org/abs/0712.0272
dc.identifierEurophys.Lett.82:69001,2008
dc.identifierdoi:10.1209/0295-5075/82/69001
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/204921
dc.subjectGeneral Relativity and Quantum Cosmology
dc.subjectAstrophysics
dc.subjectHigh Energy Physics - Theory
dc.titleInstability of scalar perturbation in a phantomic cosmological scenario
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