2005
DOI: 10.1016/j.nuclphysb.2005.07.022
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Avoidance of big rip in phantom cosmology by gravitational back reaction

Abstract: The effects of the gravitational back reaction of cosmological perturbations are investigated in a cosmological model where the universe is dominated by phantom energy. We assume a COBE normalized spectrum of cosmological fluctuations at the present time and calculate the effective energy-momentum tensor of the gravitational back-reactions of cosmological perturbations whose wavelengths at the time when the back-reactions are evaluated are larger than the Hubble radius.Our results reveal that the effects of gr… Show more

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Cited by 93 publications
(32 citation statements)
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“…For γ m ≃ 1, we expect at the transition timeḢ = 0, the kinetic energy of quintom field be of the same order of magnitude as dark matter density, see eq. (8). Using this conclusion in eq.…”
Section: Resultsmentioning
confidence: 86%
“…For γ m ≃ 1, we expect at the transition timeḢ = 0, the kinetic energy of quintom field be of the same order of magnitude as dark matter density, see eq. (8). Using this conclusion in eq.…”
Section: Resultsmentioning
confidence: 86%
“…This is the analogous of asking about the age of the universe, determined by our distance to the original Big Bang singularity. Nevertheless, in the same way as we do not expect the Big Bang singularity to exist actually, but rather being regularized by some quantum effects, by high curvature corrections to Einstein's gravity or even by varying physical constants [33], we do not expect the future singularities to be physical, at least the strongest types where physical quantities diverge [34][35][36][37]. However, it will be useful to have some estimation on how close to us a given singularity can be and, therefore, have an idea of how far in the future we could extrapolate a model with a certain type of future singularity.…”
Section: Introductionmentioning
confidence: 80%
“…Examples include the so-called "X-matter" (Turner & White 1997;Zhu et al 2001;Alcaniz et al 2003b;Dai et al 2004;Rupetti et al 2007;Wang et al 2007), a decaying vacuum energy density or a time varying Λ-term (Ozer & Taha 1987;Vishwakarma 2001), an evolving scalar field, dubbed quintessence (Ratra & Peebles 1988;Caldwell et al 1988;Wang & Lovelace 2001;Gong 2002;Chen & Ratra 2004;Choudhury & Padmanabhan 2005;Ichikawa et al 2006), the phantom energy, in which the sum of the pressure and energy density is negative (Caldwell 2002;Dabrowski et al 2003;Wang et al 2004;Wu & Yu 2005Chang et al 2007), the Chaplygin gas (Kamenshchik et al 2001;Bento et al 2002;Alam et al 2003;Alcaniz et al 2003a;Dev et al 2003;Silva & Bertolami 2003;Makler et al 2003;Zhu 2004;), the quintom model Guo et al 2005;Zhao et al 2005;Xia et al 2006;Wei & Zhang 2007), the holographic dark energy (Li 2004;Zhang & Wu 2005;Chang et al 2006), the Cardassion model (Freese & Lewis 2002;Zhu & Fujimoto 2002Sen & Sen 2003;Wang et al 2003;Gong & Duan 2004a...…”
Section: Conclusion and Discussionmentioning
confidence: 99%