Scrutinizing various phenomenological interactions in the context of holographic Ricci dark energy models

Sadri, Ehsan; Khurshudyan, Martiros; Zeng, Ding-fang

doi:10.1140/epjc/s10052-020-7983-x

Cited by 21 publications

(7 citation statements)

References 117 publications

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“…In particular, we see that, when H 0 = 67.40±0.5 km s −1 Mpc −1 , the GPs reconstruction of Eq. (23) shows that the second Swampland criteria, Eq. ( 11), for a dark energy dominated Universe, will not be satisfied.…”

Section: Swampland With Fmentioning

confidence: 99%

“…In modern cosmology, the interest in dark energy comes from the possibility to generate a negative pressure, able to accelerate the expansion of the Universe. The goal of this paper does not go in the direction of dark energy and thus, correspondingly, we will suppress any further discussion of it, referring the readers to [18][19][20][21][22][23][24][25][26][27][28][29][30] and to the references at the end of this paper, for more information.…”

Section: Introductionmentioning

confidence: 99%

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Swampland criteria for f(R) gravity derived with a Gaussian process

Elizalde

Khurshudyan

2022

Eur. Phys. J. C

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A Gaussian Process (GP) is used to derive Swampland criteria for f(R) modifications of General Relativity (GR). The fact that observational data are directly taken into account allows obtaining clean upper and lower limits for the Swampland criteria, in an unbiased, natural way. They correspond to a dark-energy dominated Universe, having assumed the form of the f(R) gravity, only. To perform this study, 40-point H(z) data are used, consisting of 30-point samples deduced from the differential age method, and 10-point additional samples coming from the radial BAO method. The constraints obtained for each f(R) model parameter choice indicate whether it is possible to alleviate the $$H_{0}$$ H 0 tension problem efficiently due to the used $$H_{0}$$ H 0 values reported by the Planck and Hubble missions. The elaborated structure of the analysis forced to limit the number of specific models, but the methodology here discussed is applicable to study any form of f(R) gravity.

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Section: Swampland With Fmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Swampland criteria for f(R) gravity derived with a Gaussian process

Elizalde

Khurshudyan

2022

Eur. Phys. J. C

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“…where the "dot" represents the derivative w.r.t. cosmic time t, and the phenomenal term Γ represents the interaction between dark matter and DE (it also gives the flow of energy between the two fluids) and has different mathematical values for both the linear and nonlinear cases, among which some linear cases are Γ 1 = 3Hb 2 ðρ m + ρ d Þ, Γ 2 = 3Hb 2 ρ m , and Γ 3 = 3Hb 2 ρ d [49][50][51][52][53][54] while some nonlinear cases are Γ 4 = 3 53,54] with b 2 being the coupling constant. We have chosen Γ = 3Hb 2 ρ m [49] as it is simple and leads to precise results.…”

Section: Kaniadakis Holographic Dark Energymentioning

confidence: 99%

Cosmic Consequences of Kaniadakis and Generalized Tsallis Holographic Dark Energy Models in the Fractal Universe

Jawad

Sultan

2021

Advances in High Energy Physics

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We investigate the recently proposed holographic dark energy models with the apparent horizon as the IR cutoff by assuming Kaniadakis and generalized Tsallis entropies in the fractal universe. The implications of these models are discussed for both the interacting ( Γ = 3 H b 2 ρ m ) and noninteracting ( b 2 = 0 ) cases through different cosmological parameters. Accelerated expansion of the universe is justified for both models through deceleration parameter q . In this way, the equation of state parameter ω d describes the phantom and quintessence phases of the universe. However, the coincidence parameter r ~ = Ω m / Ω d shows the dark energy- and dark matter-dominated eras for different values of parameters. It is also mentioned here that the squared speed of sound gives the stability of the model except for the interacting case of the generalized Tsallis holographic dark energy model. It is mentioned here that the current dark energy models at the apparent horizon give consistent results with recent observations.

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“…On the other hand, available observational data do provide some hints, partially shedding light on this dark energy problem. Nowadays, from the observational data alone, in a model-independent way, it is possible to decide what are the directions to look for, and the possible candidates for dark energy to be seriously considered, in order to solve the accelerated expanding Universe problems (for dark energy models with fluids, see [14][15][16][17][18][19][20][21][22][23][24][25][26][27][28] and references therein).…”

Section: Introductionmentioning

confidence: 99%

“…We refer the readers to[14][15][16][17][18][19][20][21][22][23][24][25][26][27][28] and references therein for further detailed discussion about fluid dark energy with related problems and its possible resolution.…”

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confidence: 99%

Analysis of the H0 tension problem in the Universe with viscous dark fluid

et al. 2020

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Two inhomogeneous single-fluid models for the Universe, which are able to naturally solve the H 0 tension problem, are discussed. The analysis is based on a Bayesian Machine Learning approach that uses a generative process. The method here adopted allows for constraint of the free parameters of each model by making use of the model itself only. The observable is taken to be the Hubble parameter, obtained from the generative process. Using the full advantages of our method, the models are constrained for two redshift ranges. Namely, first this is done with mock HðzÞ data over z ∈ ½0; 2.5, thus covering known HðzÞ observational data, which are most helpful to validate the fit results. Then, aiming to extend to redshift ranges to be covered by the most recent ongoing and future planned missions, the models are constrained for the range z ∈ ½0; 5, too. Full validation of the results for this extended redshift range will have to wait for some years, for when higher-redshift HðzÞ data become available. This makes our models fully falsifiable. In addition, our second model is able to explain the BOSS reported value for HðzÞ at z ¼ 2.34.

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Scrutinizing various phenomenological interactions in the context of holographic Ricci dark energy models

Abstract: studied the jerk parameter for all models. Using our modified CAMB code, we observed that the interacting models suppress the CMB spectrum at low multipoles and enhances the acoustic peaks.

Cited by 21 publications

References 117 publications

Swampland criteria for f(R) gravity derived with a Gaussian process

Swampland criteria for f(R) gravity derived with a Gaussian process

Cosmic Consequences of Kaniadakis and Generalized Tsallis Holographic Dark Energy Models in the Fractal Universe

Analysis of the H0 tension problem in the Universe with viscous dark fluid

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