Clustering Properties of Dynamical Dark Energy Models

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dc.creatorAvelino, P. P.
dc.creatorBeca, L. M. G.
dc.creatorMartins, C. J. A. P.
dc.date2008-02-01
dc.date.accessioned2026-07-07T11:40:06Z
dc.date.available2026-07-07T11:40:06Z
dc.descriptionWe provide a generic but physically clear discussion of the clustering properties of dark energy models. We explicitly show that in quintessence-type models the dark energy fluctuations, on scales smaller than the Hubble radius, are of the order of the perturbations to the Newtonian gravitational potential, hence necessarily small on cosmological scales. Moreover, comparable fluctuations are associated with different gauge choices. We also demonstrate that the often used homogeneous approximation is unrealistic, and that the so-called dark energy mutation is a trivial artifact of an effective, single fluid description. Finally, we discuss the particular case where the dark energy fluid is coupled to dark matter.
dc.description5 pages
dc.identifierhttps://arxiv.org/abs/0802.0174
dc.identifierhttp://arxiv.org/abs/0802.0174
dc.identifierPhys.Rev.D77:101302,2008
dc.identifierdoi:10.1103/PhysRevD.77.101302
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/200151
dc.subjectAstrophysics
dc.titleClustering Properties of Dynamical Dark Energy Models
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