Modeling holographic dark energy with particle and future horizons

Cruz, Miguel; Lepe, Samuel

doi:10.1016/j.nuclphysb.2020.115017

Cited by 18 publications

(11 citation statements)

References 56 publications

(77 reference statements)

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“…See for instance the Refs. [63,64] where the introduction of chemical potential in models beyond the standard cosmology resolves the negativity problem of entropy or temperature in a phantom scenario.…”

Section: Thermodynamicsmentioning

confidence: 99%

Non-zero torsion and late cosmology

2020

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In this work, we study some thermodynamical aspects associated with torsion in a flat FLRW spacetime cosmic evolution. By implementing two Ansatze for the torsion term, we find that the model admits a phantom regime or a quintessence behavior. This scheme differs from the CDM model at the thermodynamical level. The resulting cosmic expansion is not adiabatic, the fulfillment of the second law of thermodynamics requires a positive torsion term, and the temperature of the cosmic fluid is always positive. The entropy of the torsion phantom scenario is negative, but introducing chemical potential solves this issue. For a Dirac-Milne type Universe, the torsion leads to a growing behavior for the temperature of the fluid but has no incidence on the rate of expansion.

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Section: Thermodynamicsmentioning

confidence: 99%

Non-zero torsion and late cosmology

2020

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“…As can be seen from equation ( 4), the parameter state depends on the cosmological redshift, for the Model I we can obtain the explicit expression for this parameter state by means of the Eqs. ( 4), (11) and the definition given above for the θ(z) function, yielding [27]…”

Section: Thermodynamics Of the Interacting Scenariomentioning

confidence: 99%

“…Of course, the election of the characteristic length is not unique, see for instance Refs. [11][12][13][14][15][16][17][18][19][20][21], where some different forms of L can be found. In Ref.…”

Section: Introductionmentioning

confidence: 99%

Holographic dark energy in curved spacetime for interacting fluids

Bolaños¹,

Crúz²,

Lepe³

et al. 2021

Preprint

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In this work we explore some aspects of two holographic models for dark energy within the interacting scenario for the dark sector with the inclusion of spatial curvature. A statistical analysis for each holographic model is performed together with their corresponding extensions given by the consideration of massive neutrinos. The first holographic approach considers the usual formula proposed by Li for the dark energy density with a constant parameter c and for the second model we have a function c(z) instead a constant parameter, this latter model is inspired in the apparent horizon. By considering the best fit values of the cosmological parameters we show that the interaction term for each holographic model, Q, keeps positive along the cosmic evolution and exhibits a future singularity for a finite value of the redshift, this is inherited from the Hubble parameter.The temperatures for the components of the dark sector are computed and have a growing behavior in both models. The cosmic evolution in this context it is not adiabatic and the second law it is fulfilled only under certain well-established conditions for the temperatures of the cosmic components and the interacting Q-term.

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“…Let us note that although the cosmological constant provides the convincing explanation for the observed accelerated expansion, a clear justification of its small value does not exist until now [49].…”

Section: Introductionmentioning

confidence: 95%

“…In [48] a holographic dark energy model has been constructed for the apparent horizon in a curved universe. The holographic models for the particle and future horizons have been analyzed in [49] with the conclusion that the future horizon presents more similarities with the dark energy behavior.…”

Section: Introductionmentioning

confidence: 99%

Spacetime Symmetry and LemaîTre Class Dark Energy Models

Dymnikova

Dobosz

2019

Symmetry

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We present the regular cosmological models of the Lemaître class with time-dependent and spatially inhomogeneous vacuum dark energy, which describe relaxation of the cosmological constant from its value powering inflation to the final non-zero value responsible for the present acceleration in the frame of one self-consistent theoretical scheme based on the algebraic classification of stress-energy tensors and spacetime symmetry directly related to their structure. Cosmological evolution starts with the nonsingular non-simultaneous de Sitter bang, followed by the Kasner-type anisotropic expansion, and goes towards the present de Sitter state. Spacetime symmetry provides a mechanism of reducing cosmological constant to a certain non-zero value involving the holographic principle which singles out the special class of the Lemaître dark energy models with the global structure of the de Sitter spacetime. For this class cosmological evolution is guided by quantum evaporation of the cosmological horizon whose dynamics entirely determines the final value of the cosmological constant. For the choice of the density profile modeling vacuum polarization in a spherical gravitational field and the GUT scale for the inflationary value of cosmological constant, its final value agrees with that given by observations. Anisotropy grows quickly at the postinflationary stage, then remains constant and decreases to A < 10 − 6 when the vacuum density starts to dominate.

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Modeling holographic dark energy with particle and future horizons

Cited by 18 publications

References 56 publications

Non-zero torsion and late cosmology

Non-zero torsion and late cosmology

Holographic dark energy in curved spacetime for interacting fluids

Spacetime Symmetry and LemaîTre Class Dark Energy Models

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