Cosmological future singularities in interacting dark energy models

Jiménez, Jose Beltrán; Rubiera-García, Diego; Sáez-Gómez, Diego; Salzano, Vincenzo

doi:10.1103/physrevd.94.123520

Cited by 33 publications

(24 citation statements)

References 119 publications

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“…The properties of dark energy are crucial for the future evolution of the universe and its eventual fate. At this respect, some models predict the existence of future singularities that can be broadly classified according to the divergence of some cosmological quantity (see for instance [52,262,126,93,160,81,62,11] for some related literature). It is indeed common to perform such a classification attending to which derivative of the scale factor diverges first [161].…”

Section: Late-time Cosmologymentioning

confidence: 99%

Born–Infeld inspired modifications of gravity

et al. 2018

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General Relativity has shown an outstanding observational success in the scales where it has been directly tested. However, modifications have been intensively explored in the regimes where it seems either incomplete or signals its own limit of validity. In particular, the breakdown of unitarity near the Planck scale strongly suggests that General Relativity needs to be modified at high energies and quantum gravity effects are expected to be important. This is related to the existence of spacetime singularities when the solutions of General Relativity are extrapolated to regimes where curvatures are large. In this sense, Born-Infeld inspired modifications of gravity have shown an extraordinary ability to regularise the gravitational dynamics, leading to non-singular cosmologies and regular black hole spacetimes in a very robust manner and without resorting to quantum gravity effects. This has boosted the interest in these theories in applications to stellar structure, compact objects, inflationary scenarios, cosmological singularities, and black hole and wormhole physics, among others. We review the motivations, various formulations, and main results achieved within these theories, including their observational viability, and provide an overview of current open problems and future research opportunities.

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Section: Late-time Cosmologymentioning

confidence: 99%

Born–Infeld inspired modifications of gravity

et al. 2018

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“…In order to solve this problem, many approaches emerged [5][6][7][8]. One interesting suggestion was a diffusive exchange of energy between dark energy and dark matter made by Calogero [9,10], Haba et al [11], and Szydlowski and Stachowski [12], with some solution to cosmic problems.…”

Section: Introductionmentioning

confidence: 99%

Interacting diffusive unified dark energy and dark matter from scalar fields

Benisty

Guendelman

2017

Eur. Phys. J. C

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Here we generalize ideas of unified dark matterdark energy in the context of two measure theories and of dynamical space time theories. In two measure theories one uses metric independent volume elements and this allows one to construct unified dark matter-dark energy, where the cosmological constant appears as an integration constant associated with the equation of motion of the measure fields. The dynamical space-time theories generalize the two measure theories by introducing a vector field whose equation of motion guarantees the conservation of a certain Energy Momentum tensor, which may be related, but in general is not the same as the gravitational Energy Momentum tensor. We propose two formulations of this idea: (I) by demanding that this vector field be the gradient of a scalar, (II) by considering the dynamical space field appearing in another part of the action. Then the dynamical space time theory becomes a theory of Diffusive Unified dark energy and dark matter. These generalizations produce non-conserved energy momentum tensors instead of conserved energy momentum tensors which leads at the end to a formulation of interacting DE-DM dust models in the form of a diffusive type interacting Unified dark energy and dark matter scenario. We solved analytically the theories for perturbative solution and asymptotic solution, and we show that the CDM is a fixed point of these theories at large times. Also a preliminary argument as regards the good behavior of the theory at the quantum level is proposed for both theories.

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“…We would like to mention that the singularities occurring in Refs. [14] and [15] have not been observed during the presented study.…”

Section: Introductionmentioning

confidence: 64%

Cosmology with an interacting van der Waals fluid

Elizalde

Khurshudyan

2018

Int. J. Mod. Phys. D

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A model for the late-time accelerated expansion of the universe is considered where a van der Waals fluid interacting with matter plays the role of dark energy. The transition towards this phase in the cosmic evolution history is discussed in detail and, moreover, a complete classification of the future finite-time singularities is obtained for six different possible forms of the non-gravitational interaction between dark energy (the van der Waals fluid) and dark matter. This study shows, in particular, that a universe with a non-interacting three-parameter van der Waals fluid can evolve into a universe characterized by a Type IV (Generalized Sudden) Singularity. On the other hand, for certain values of the parameters, exit from the accelerated expanding phase is possible in the near future, what means that the expansion of the universe in the future could become decelerated. On the other hand, our study shows that space can be divided into different regions. For some of them, in particular, the non-gravitational interactions Q = 3Hbρ de , Q = 3Hbρ dm and Q = 3Hb(ρ de + ρ de ) may completely suppress future finite-time singularity formation, for sufficiently high values of b. On the other hand, for some other regions of the parameter space, the mentioned interactions would not affect the singularity type, namely the Type IV singularity generated in the case of the non-interacting model would be preserved. A similar conclusion has been archived for the cases of Q = 3bHρ de ρ dm /(ρ de + ρ dm ), Q = 3bHρ 2 dm /(ρ de +ρ dm ) and Q = 3bHρ 2 de /(ρ de +ρ dm ) non-gravitational interactions, with only one difference: the Q = 3bHρ 2 dm /(ρ de +ρ dm ) interaction will change the Type IV singularity of the non-interacting model into a Type II (The Sudden) singularity. *

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Cosmological future singularities in interacting dark energy models

Cited by 33 publications

References 119 publications

Born–Infeld inspired modifications of gravity

Born–Infeld inspired modifications of gravity

Interacting diffusive unified dark energy and dark matter from scalar fields

Cosmology with an interacting van der Waals fluid

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