Holographic Dark Energy From a Modified Gbig Scenario

Nozari, Kourosh; Rashidi, Narges

doi:10.1142/s021827181001635x

Cited by 24 publications

(20 citation statements)

References 77 publications

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“…28 Table 9: Constraints on the e-folds number and temperature during the reheating phase in the GB model with canonical scalar field and with V = V 0 φ n and G = G 0 φ −n , obtained from Planck2018 TT, TE, EE+lowE+lensing+BK14+BAO joint data. In this case, we use the potential and GB coupling defined in equation (29). As we have seen before, in this case the GB model only with n = 2 is consistent with the base data.…”

Section: Reheating Phase In a Gauss-bonnet Model With Canonical Scalasupporting

confidence: 62%

Gauss–Bonnet Inflation after Planck2018

Rashidi

Nozari

2020

ApJ

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We study the primordial perturbations and reheating process in the models where the Gauss-Bonnet term is non-minimally coupled to the canonical and non-canonical (DBI and tachyon) scalar fields. We consider several potentials and Gauss-Bonnet coupling terms as power-law, dilaton-like, cosh-type, E-model and T-model. To seek the observational viability of these models, we study the scalar perturbations numerically and compare the results with the Planck2018 TT, TE, EE+lowE+lensing+BK14+BAO joint data at 68% CL and 95% CL. We also study the tensor perturbations in confrontation with the Planck2018 TT, TE, EE+lowE+lensing+BK14+BAO+ LIGO&Virgo2016 joint data at 68% CL and 95% CL. In this regard, we obtain some constraints on the Gauss-Bonnet coupling parameter β. Another important process in the early universe is the reheating phase after inflation which is necessary to reheat the universe for subsequent evolution. In this regard, we study the reheating process in these models and find some expressions for the e-folds number and temperature during that era. Considering that from Planck TT,TE,EE+lowEB+lensing data and BICEP2/Keck Array 2014, based on the ΛCDM+r + dns d ln k model, we have n s = 0.9658 ± 0.0038 and r < 0.072, we obtain some constraints on the e-folds number and temperature. From the values of the e-folds number and the effective equation of state and also the observationally viable value of the scalar spectral index, we explore the capability of the models in explaining the reheating phase. PACS: 98.80. Bp, 98.80.Cq, 98.80.Es

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Section: Reheating Phase In a Gauss-bonnet Model With Canonical Scalasupporting

confidence: 62%

Gauss–Bonnet Inflation after Planck2018

Rashidi

Nozari

2020

ApJ

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“…We now want to calculate the values of ω 0 and ω 1 for three different values of the running parameter Inserting in Eqs. (112) and (113) the values of the parameters involved, we obtain, for λ = 1.02:…”

Section: Non Interacting Casementioning

confidence: 99%

Power-law entropy-corrected holographic dark energy in Hořava-Lifshitz cosmology with Granda-Oliveros cut-off

Pasqua

Chattopadhyay²,

Myrzakulov

2016

Eur. Phys. J. Plus

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In this paper, we study the Power Law Entropy Corrected Holographic Dark Energy (PLECHDE) model in the framework of a non-flat Universe and of Hořava-Lifshitz cosmology with infrared cut-off given by recently proposed Granda-Oliveros cut-off, which contains one term proportional to the Hubble parameter squared H 2 and one term proportional to the first time derivative of the Hubble parameterḢ. Moreover, this cut-off is characterized by two constant parameters, α and β. For the two cases corresponding to noninteracting and interacting DE and Dark Matter (DM), we derive the evolutionary form of the energy density of DE Ω ′ D , the Equation of State (EoS) parameter of DE ω D and the deceleration parameter q. Using the parametrization of the EoS parameter ω D (z) = ω 0 + ω 1 z,we obtain the expressions of the two parameters ω 0 and ω 1 . We also study the statefinder parameters {r, s}, the snap and lerk cosmographic parameters and the squared speed of the sound v 2 s . We also calculate the values of the quantities we study for different values of the running parameter λ and for different set of values of α and β.

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“…Different versions of the cutoff corresponding to generalized holographic dark energy [25] have been considered in Refs. [26][27][28][29][30][31][32][33][34][35][36][37][38][39][40][41].…”

Section: Introductionmentioning

confidence: 99%

Covariant generalized holographic dark energy and accelerating universe

2017

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We propose the generalized holographic dark energy model where the infrared cutoff is identified with the combination of the FRW universe parameters: the Hubble rate, particle and future horizons, cosmological constant, the universe lifetime (if finite) and their derivatives. It is demonstrated that with the corresponding choice of the cutoff one can map such holographic dark energy to modified gravity or gravity with a general fluid. Explicitly, F(R) gravity and the general perfect fluid are worked out in detail and the corresponding infrared cutoff is found. Using this correspondence, we get realistic inflation or viable dark energy or a unified inflationary-dark energy universe in terms of covariant holographic dark energy.

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Holographic Dark Energy From a Modified Gbig Scenario

Cited by 24 publications

References 77 publications

Gauss–Bonnet Inflation after Planck2018

Gauss–Bonnet Inflation after Planck2018

Power-law entropy-corrected holographic dark energy in Hořava-Lifshitz cosmology with Granda-Oliveros cut-off

Covariant generalized holographic dark energy and accelerating universe

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