Turbulence accelerating cosmology from an inhomogeneous dark fluid

Brevik, Iver; Тимошкин, А. В.; Rabochaya, Y.; Zerbini, Sergio

doi:10.1007/s10509-013-1506-2

Cited by 8 publications

(6 citation statements)

References 43 publications

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“…In the following we will consider a dark fluid developing into the future from the present time t = 0, when turbulence is accounted for. We will perform the analysis in two different ways: either assuming a two-fluid model with one turbulent constituent, or assuming simply a one-component fluid, following [9,68,152,153].…”

Section: Inclusion Of Isotropic Turbulencementioning

confidence: 99%

Viscous cosmology for early- and late-time universe

Brevik

Grøn

Haro

et al. 2017

Int. J. Mod. Phys. D

211

137

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point of view the inclusion of viscosity concepts in the macroscopic theory of the cosmic fluid would appear most natural, as an ideal fluid is after all an abstraction (exluding special cases such as superconductivity). Making use of modern observational results for the Hubble parameter plus standard Friedmann formalism, we may extrapolate the description of the universe back in time up to the inflationary era, or we may go to the opposite extreme and analyze the probable ultimate fate of the universe. In this review, we discuss a variety of topics in cosmology when it is enlarged in order to contain a bulk viscosity. Various forms of this viscosity, when expressed in terms of the fluid density or the Hubble parameter, are discussed. Furthermore, we consider homogeneous as well as inhomogeneous equations of state. We investigate viscous cosmology in the early universe, examining the viscosity effects on the various inflationary observables. Additionally, we study viscous cosmology in the late universe, containing current acceleration and the possible future singularities, and we investigate how one may even unify inflationary and late-time acceleration. Finally, we analyze the viscosity-induced crossing through the quintessence-phantom divide, we examine the realization of viscosity-driven cosmological bounces, and we briefly discuss how the Cardy–Verlinde formula is affected by viscosity.\ud © 2017 World Scientific Publishing Company From a hydrodynamicist’sPeer ReviewedPostprint (author's final draft

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Section: Inclusion Of Isotropic Turbulencementioning

confidence: 99%

Viscous cosmology for early- and late-time universe

Brevik

Grøn

Haro

et al. 2017

Int. J. Mod. Phys. D

211

137

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“…The natural conclusion here is that the situation is too complex to apply the simple estimates made use of in common kinetic theory. The expression (11) should not be abandoned on physical grounds. Actually, the constant bulk viscosity model has quite frequently been made use of in the literature.…”

Section: The Laminar Epochmentioning

confidence: 99%

“…Refs. [11,12,13]. Making use of the viscoelastic analogy, we will have the opportunity to calculate the entropy production at the transition.…”

Section: Introductionmentioning

confidence: 99%

Temperature variation in the dark cosmic fluid in the late universe

Brevik

2016

Mod. Phys. Lett. A

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A one-component dark energy fluid model of the late universe is considered (w < −1) when the fluid, initially assumed laminar, makes a transition into a turbulent state of motion. Spatial isotropy is assumed so that only the bulk viscosities are included (ζ in the laminar epoch and ζ turb in the turbulent epoch). Both viscosities are assumed to be constants. We derive a formula, new as far as we know, for the time dependence of the temperature T (t) in the laminar case when viscosity is included. Assuming that the laminar/turbulent transition takes place at some time t s before the big rip is reached, we then analyze the positive temperature jump experienced by the fluid at t = t * if ζ turb > ζ. This is just as one would expect physically. The corresponding entropy production is also considered. A special point emphasized in the paper is the analogy that exists between the cosmic fluid and a so-called Maxwell fluid in viscoelasticity.PACS numbers: 95.36.+x, 47.27.Gs

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“…Unlike a model containing only a pure dark energy, the presence of an interaction term between dark energy and dark matter in the gravitational equations leads to corrections in the EoS parameters; see Refs. [25,26,27,28]. The case of the very early universe was emphasized.…”

Section: Discussionmentioning

confidence: 99%

Little Rip and Pseudo Rip Phenomena From Coupled Dark Energy

2013

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We consider Little Rip (LR) and Pseudo Rip (PR) cosmological models with two interacting ideal fluids, corresponding to dark energy and dark matter. The interaction between the dark energy and the dark matter fluid components is described in terms of the parameters in the equations of state for the LR and PR universes. In contrast to a model containing only a pure dark energy, the presence of the interaction term between the fluid components in the gravitational equations leads to a modification of the equation of state parameters. The properties of the early universe in this formalism are pointed out.

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Turbulence accelerating cosmology from an inhomogeneous dark fluid

Cited by 8 publications

References 43 publications

Viscous cosmology for early- and late-time universe

Viscous cosmology for early- and late-time universe

Temperature variation in the dark cosmic fluid in the late universe

Little Rip and Pseudo Rip Phenomena From Coupled Dark Energy

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