Escaping the Big Rip?

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dc.creatorBouhmadi-Lopez, Mariam
dc.creatorMadrid, Jose A. Jimenez
dc.date2004-04-27
dc.date.accessioned2026-07-07T10:47:51Z
dc.date.available2026-07-07T10:47:51Z
dc.descriptionWe discuss dark energy models which might describe effectively the actual acceleration of the universe. More precisely, for a 4-dimensional Friedmann-Lema\^ıtre-Robertson-Walker (FLRW) universe we consider two situations: First of them, we model dark energy by phantom energy described by a perfect fluid satisfying the equation of state $P=(β-1)ρ$ (with $β<0$ and constant). In this case the universe reaches a ``Big Rip'' independently of the spatial geometry of the FLRW universe. In the second situation, the dark energy is described by a phantom (generalized) Chaplygin gas which violates the dominant energy condition. Contrary to the previous case, for this material content a FLRW universe would never reach a ``big rip'' singularity (indeed, the geometry is asymptotically de Sitter). We also show how this dark energy model can be described in terms of scalar fields, corresponding to a minimally coupled scalar field, a Born-Infeld scalar field and a generalized Born-Infeld scalar field. Finally, we introduce a phenomenologically viable model where dark energy is described by a phantom generalized Chaplygin gas.
dc.description12 pages, 11 figures, RevTeX 4
dc.identifierhttps://arxiv.org/abs/astro-ph/0404540
dc.identifierhttp://arxiv.org/abs/astro-ph/0404540
dc.identifierJCAP0505:005,2005
dc.identifierdoi:10.1088/1475-7516/2005/05/005
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/183677
dc.subjectAstrophysics
dc.titleEscaping the Big Rip?
dc.typetext

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