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Matter Growth in Imperfect Fluid Cosmology

PPGCosmo & Núcleo Cosmo-UFES, Universidade Federal do Espírito Santo, Av. Fernando Ferrari, 514, Campus de Goiabeiras, CEP 29075-910 Vitória, Espírito Santo, Brazil
Departamento de Física, Universidade Federal de Ouro Preto (UFOP), CEP 35400-000 Ouro Preto, Minas Gerais, Brazil
Departamento de Física, Universidade Federal do Paraná, 81531-980 Curitiba, Paraná, Brazil
Author to whom correspondence should be addressed.
These authors contributed equally to this work.
Universe 2019, 5(3), 68;
Received: 2 November 2018 / Revised: 24 February 2019 / Accepted: 25 February 2019 / Published: 4 March 2019
PDF [628 KB, uploaded 4 March 2019]


Extensions of Einstein’s General Relativity (GR) can formally be given a GR structure in which additional geometric degrees of freedom are mapped on an effective energy-momentum tensor. The corresponding effective cosmic medium can then be modeled as an imperfect fluid within GR. The imperfect fluid structure allows us to include, on a phenomenological basis, anisotropic stresses and energy fluxes which are considered as potential signatures for deviations from the cosmological standard Λ -cold-dark-matter ( Λ CDM) model. As an example, we consider the dynamics of a scalar-tensor extension of the standard model, the e Φ Λ CDM model. We constrain the magnitudes of anisotropic pressure and energy flux with the help of redshift-space distortion (RSD) data for the matter growth function f σ 8 . View Full-Text
Keywords: fluid cosmology; cosmological perturbation theory; scalar-tensor theory; cosmic structure formation fluid cosmology; cosmological perturbation theory; scalar-tensor theory; cosmic structure formation

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Zimdahl, W.; Velten, H.E.; Algoner, W.C. Matter Growth in Imperfect Fluid Cosmology. Universe 2019, 5, 68.

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