2021
DOI: 10.1140/epjc/s10052-021-09177-7
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Growth of matter perturbations in the extended viscous dark energy models

Abstract: In this work, we study the extended viscous dark energy models in the context of matter perturbations. To do this, we assume an alternative interpretation of the flat Friedmann–Lemaître–Robertson–Walker Universe, through the nonadditive entropy and the viscous dark energy. We implement the relativistic equations to obtain the growth of matter fluctuations for a smooth version of dark energy. As result, we show that the matter density contrast evolves similarly to the $$\Lambda $$ Λ … Show more

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Cited by 15 publications
(15 citation statements)
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References 132 publications
(137 reference statements)
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“…The bulk viscosity can be a thermodynamic function ξ(t) = η 0 ρ ν DE , as introduced in reference [344]. A fit to the combination of Planck 2018 CMB distance priors + Pantheon + BAO + BBN + CC data on this model gives H 0 = 69.2 ± 1.7 km s −1 Mpc −1 at 68% CL [340], alleviating the Hubble tension down to 1.9σ as in the two previous models. Note that a CMB-only analysis for all these models is currently missing.…”
Section: Bulk Viscous Modelsmentioning
confidence: 69%
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“…The bulk viscosity can be a thermodynamic function ξ(t) = η 0 ρ ν DE , as introduced in reference [344]. A fit to the combination of Planck 2018 CMB distance priors + Pantheon + BAO + BBN + CC data on this model gives H 0 = 69.2 ± 1.7 km s −1 Mpc −1 at 68% CL [340], alleviating the Hubble tension down to 1.9σ as in the two previous models. Note that a CMB-only analysis for all these models is currently missing.…”
Section: Bulk Viscous Modelsmentioning
confidence: 69%
“…Considering that DE has a viscous nature, where the viscosity coefficient is proportional to the Hubble parameter ξ(t) = η 0 H, as introduced in reference [339], the authors of reference [340] have found that for this model, the combination of Planck 2018 CMB distance priors + Pantheon + BAO + BBN + CC results in H 0 = 69.3 ± 1.7 km s −1 Mpc −1 at 68% CL, reducing the Hubble tension to the 1.9σ level.…”
Section: Bulk Viscous Modelsmentioning
confidence: 99%
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“…The cosmological scenarios in which a fluid is endowed with a bulk viscosity is an effective description to alleviate the Hubble constant tension [683][684][685]. A bulk viscous fluid is characterized by its energy density ρ and pressure p where this pressure term has two distinct components, namely, p = p u +p vis .…”
Section: Bulk Viscous Modelsmentioning
confidence: 99%
“…Thus, one can see that for different choices of the bulk viscous coefficient, ξ(t), one can extract the constraints out of various cosmological scenarios. The cosmic fluid endowed by the bulk viscosity can either represent a DE fluid [685] or a unified fluid which combines both DM and DE behaviours [684]. The cosmological scenarios in which DE enjoys a viscous nature have been investigated in the literature aiming to address the Hubble tension [687][688][689][690].…”
Section: Bulk Viscous Modelsmentioning
confidence: 99%