Phantom and non-phantom dark energy: The cosmological relevance of non-locally corrected gravity

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dc.creatorJhingan, S.
dc.creatorNojiri, S.
dc.creatorOdintsov, S. D.
dc.creatorSami, M.
dc.creatorThongkool, I
dc.creatorZerbini, S.
dc.date2008-03-18
dc.date2008-04-21
dc.date.accessioned2026-07-07T11:33:14Z
dc.date.available2026-07-07T11:33:14Z
dc.descriptionIn this paper we have investigated the cosmological dynamics of non-locally corrected gravity involving a function of the inverse d'Alembertian of the Ricci scalar, $f(\Box^{-1} R))$. Casting the dynamical equations into local form, we derive the fixed points of the dynamics and demonstrate the existence and stability of a one parameter family of dark energy solutions for a simple choice, $f(\Box^{-1} R)\sim \exp(α\Box^{-1} R)$. The effective EoS parameter is given by, $w_{\rm eff}=({α-1})/({3α-1})$ and the stability of the solutions is guaranteed provided that $1/3<α<2/3$. For $1/3<α<1/2$ and $1/2<α<2/3$, the underlying system exhibits phantom and non-phantom behavior respectively; the de Sitter solution corresponds to $α=1/2$. For a wide range of initial conditions, the system mimics dust like behavior before reaching the stable fixed point. The late time phantom phase is achieved without involving negative kinetic energy fields. A brief discussion on the entropy of de Sitter space in non-local model is included.
dc.description5 pages and 2 figures, typos corrected, final version to appear in Phys. Lett. B
dc.identifierhttps://arxiv.org/abs/0803.2613
dc.identifierhttp://arxiv.org/abs/0803.2613
dc.identifierPhys.Lett.B663:424-428,2008
dc.identifierdoi:10.1016/j.physletb.2008.04.054
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/197823
dc.subjectHigh Energy Physics - Theory
dc.subjectAstrophysics
dc.subjectGeneral Relativity and Quantum Cosmology
dc.subjectHigh Energy Physics - Phenomenology
dc.titlePhantom and non-phantom dark energy: The cosmological relevance of non-locally corrected gravity
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