The quantum realm of the ``Little Sibling'' of the Big Rip singularity

Albarran, Imanol; Bouhmadi-López, Mariam; Cabral, Francisco; Martín–Moruno, Prado

doi:10.1088/1475-7516/2015/11/044

Cited by 29 publications

(32 citation statements)

References 94 publications

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“…For the three models at hand, we can solve (A5) analytically well inside the DE dominated regime, i.e., for t ≥ t * we have H 2 ≈ (κ 2 /3)ρ d , obtaining for each case the potential [40,41,[93][94][95] …”

Section: Discussionmentioning

confidence: 99%

“…The classical singular asymptotic behaviour of these dark energy models has led to a quantum cosmological analysis of these setups [39][40][41][42]95]. In these works, it was concluded that once the Universe enters in a genuinely quantum phase; i.e., where coherence and entanglement effects are important, the Universe would evade a doomsdayà la rip.…”

Section: Introductionmentioning

confidence: 99%

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Cosmological perturbations in an effective and genuinely phantom dark energy Universe

Albarran

Bouhmadi-López

Morais

2017

Physics of the Dark Universe

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We carry out an analysis of the cosmological perturbations in general relativity for three different models which are good candidates to describe the current acceleration of the Universe. These three set-ups are described classically by perfect fluids with a phantom nature and represent deviations from the most widely accepted ΛCDM model. In addition, each of the models under study induce different future singularities or abrupt events known as (i) Big Rip, (ii) Little Rip and (iii) Little Sibling of the Big Rip. Only the first one is regarded as a true singularity since it occurs at a finite cosmic time. For this reason, we refer to the others as abrupt events. With the aim to find possible footprints of this scenario in the Universe matter distribution, we not only obtain the evolution of the cosmological scalar perturbations but also calculate the matter power spectrum for each model. We have carried the perturbations in the absence of any anisotropic stress and within a phenomenological approach for the speed of sound. We constrain observationally these models using several measurements of the growth rate function, more precisely f σ8, and compare our results with the observational ones.

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Section: Discussionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Cosmological perturbations in an effective and genuinely phantom dark energy Universe

Albarran

Bouhmadi-López

Morais

2017

Physics of the Dark Universe

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“…However, as energy density diverges in all the cases presented, one might expect that quantum effects become important at some point in the future evolution. In fact, a quantum analysis shows that in all cases, the classical abrupt event can be avoided from a quantum point of view [16][17][18][19].…”

Section: Introductionmentioning

confidence: 99%

Cosmological Perturbations in Phantom Dark Energy Models

2017

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Abstract:The ΛCDM paradigm, characterised by a constant equation of state w = −1 for dark energy, is the model that better fits observations. However, the same observations strongly support the possibility of a dark energy content where the corresponding equation of state is close to but slightly smaller than −1. In this regard, we focus on three different models where the dark energy content is described by a perfect fluid with an equation of state w −1 which can evolve or not. The three proposals show very similar behaviour at present, while the asymptotic evolution of each model drives the Universe to different abrupt events known as (i) Big Rip; (ii) Little Rip (LR); and (iii) Little Sibling of the Big Rip. With the aim of comparing these models and finding possible imprints in their predicted matter distribution, we compute the matter power spectrum and the growth rate f σ 8 . We conclude that the model which induces a LR seems to be favoured by observations.

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“…Since Equation (36) is a second order differential equation, only two of the four ϕ (i) k functions given in Equation (38) are linearly independent. These functions can be written as [44,45] …”

Section: Wdw Equation With a Scalar Fieldmentioning

confidence: 99%

The Avoidance of the Little Sibling of the Big Rip Abrupt Event by a Quantum Approach

et al. 2018

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Abstract:We address the quantisation of a model that induces the Little Sibling of the Big Rip (LSBR) abrupt event, where the dark energy content is described by means of a phantom-like fluid or a phantom scalar field. The quantisation is done in the framework of the Wheeler-DeWitt (WDW) equation and imposing the DeWitt boundary condition; i.e., the wave function vanishes close to the abrupt event. We analyse the WDW equation within two descriptions: First, when the dark energy content is described with a perfect fluid. This leaves the problem with the scale factor as the single degree of freedom. Second, when the dark energy content is described with a phantom scalar field in such a way that an additional degree of freedom is incorporated. Here, we have applied the Born-Oppenheimer (BO) approximation in order to simplify the WDW equation. In all cases, the obtained wave function vanishes when the LSBR takes place, thus fulfilling the DeWitt boundary condition.

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The quantum realm of the ``Little Sibling'' of the Big Rip singularity

Cited by 29 publications

References 94 publications

Cosmological perturbations in an effective and genuinely phantom dark energy Universe

Cosmological perturbations in an effective and genuinely phantom dark energy Universe

Cosmological Perturbations in Phantom Dark Energy Models

The Avoidance of the Little Sibling of the Big Rip Abrupt Event by a Quantum Approach

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