Holographic dark energy in Gauss-Bonnet gravity with Granda-Oliveros cut-off

Koussour, M.; Filali, H.; Shekh, S. H.; Bennai, M.

doi:10.1016/j.nuclphysb.2022.115738

Cited by 30 publications

(16 citation statements)

References 47 publications

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“…Bunn et al [37] conducted statistical analysis on 4-yr data from CMB and set a limit for primordial anisotropy to be less than 10 −3 in Planck epoch. Many researchers have used this condition to find exact solutions of field equations in many backgrounds [38,39].…”

Section: B Bmentioning

confidence: 99%

Late-time acceleration in $f\left( Q\right) $ gravity: Analysis and constraints in an anisotropic background

Koussour¹,

Bourakadi²,

Shekh³

et al. 2022

Preprint

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This paper is devoted to investigate the anisotropic locally rotationally symmetric (LRS) Bianchi type-I space-time in the context of the recently proposed f (Q) gravity in which Q is the nonmetricity scalar. For this purpose, we consider a linear form of f (Q) gravity model, specifically, f (Q) = αQ + β, where α and β are free parameters and we analyzed the exact solutions of LRS Bianchi type-I space-time. The modified Friedmann equations are solved by presuming an expansion scalar θ (t) is proportional to the shear scalar σ (t) which leads to the relation between the metric potentials as A = B n where n is an arbitrary constant. Then we constrain our model parameters with the observational Hubble datasets of 57 data points. Moreover, we discuss the physical behavior of cosmological parameters such as energy density, pressure, EoS parameter, and deceleration parameter. The behavior of the deceleration parameter predicts a transition from deceleration to accelerated phases in an expanding Universe. Finally, the EoS parameter indicates that the anisotropic fluid behaves like the standard ΛCDM model.

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Section: B Bmentioning

confidence: 99%

Late-time acceleration in $f\left( Q\right) $ gravity: Analysis and constraints in an anisotropic background

Koussour¹,

Bourakadi²,

Shekh³

et al. 2022

Preprint

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“…The physical justification for this condition is imposed on the basis of the observations of the velocity redshift relation for extragalactic sources which propose that the Hubble expansion of the Universe may achieve isotropy when σ θ is constant [48]. This condition has been used in many works [17,28].…”

Section: Lambert Function Distribution and Cosmological Solutionsmentioning

confidence: 99%

“…Another line of research has taken interest in modified gravity theories (MGT) which were introduced as a set of modifications to Einstein's general relativity which can describe the accelerated expansion without the need for an added component or exotic matter. Various theories of modified gravity were explored in the literature, mainly f (R) gravity (R is the Ricci scalar), f (G) gravity (G is the Gauss-Bonnet invariant), f (R, T) gravity (R is the Ricci scalar and T is the trace of the stress-energy tensor), and many extensive scalar-tensor theories [12][13][14][15][16][17][18]. f (Q) gravity was introduced as a symmetric teleparallel modification of gravity and has gained much interest in recent studies as it has shown many promising results in terms of compatibility with observational constraints [19][20][21][22][23][24][25][26][27][28][29][30][31][32][33][34][35].…”

mentioning

confidence: 99%

Barrow holographic dark energy models in f(Q) symmetric teleparallel gravity with Lambert function distribution

Koussour

Shekh

Filali

et al. 2022

Int. J. Geom. Methods Mod. Phys.

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The paper presents Barrow holographic dark energy (infrared cut-off is the Hubble horizon) suggested by Barrow [The area of a rough black hole, Phys. Lett. B 808 (2020) 135643] recently in an anisotropic Bianchi type-I Universe within the framework of [Formula: see text] symmetric teleparallel gravity, where the non-metricity scalar [Formula: see text] is responsible for the gravitational interaction. We consider two cases: Interacting and non-interacting models of pressureless dark matter and Barrow holographic dark energy by solving [Formula: see text] symmetric teleparallel field equations. To find the exact solutions of the field equations, we assume that the time-redshift relation follows a Lambert function distribution as [Formula: see text], where [Formula: see text], [Formula: see text] and [Formula: see text] are non-negative constants and [Formula: see text] represents the age of the Universe. Moreover, we discuss several cosmological parameters such as energy density, equation of state (EoS) and skewness parameters, squared sound speed, and [Formula: see text] plane. Finally, we found the values of the deceleration parameter (DP) for the Lambert function distribution as [Formula: see text] and [Formula: see text] which are consistent with recent observational data, i.e. DP evolves with cosmic time from initial deceleration to late-time acceleration.

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“…In the literature, there are many alternatives to GR that attempt to explain this problem [5][6][7]. The most popular alternative currently proposed are modified gravity theories such as f (R) gravity, where f (R) is an arbitrary function of the Ricci scalar R. Several models have been studied in framework of f (R) gravity in var-ious cosmological contexts [8][9][10].…”

Section: Introductionmentioning

confidence: 99%