Entropy-corrected Holographic Dark Energy Research Articles

Reconstructing extended f(P) cubic gravity from entropy-corrected holographic and new agegraphic dark energy models

This work deals with the newly approached extended [Formula: see text] cubic gravity in a cosmological background where [Formula: see text] denotes the cubic gravity. Here, we peruse the cosmological nature of the different types of dark energy candidates in the framework of [Formula: see text] gravity. Next, we study the reconstruction scenario of [Formula: see text] gravity model according to ordinary holographic dark energy, ordinary new agegraphic dark energy, entropy-corrected holographic dark energy in power-law and logarithmic versions and entropy-corrected new agegraphic dark energy in power-law and logarithmic versions with two classes of the scale factor. We derive different forms of the unknown function [Formula: see text] in the context of these dark energy candidates. By the trajectories of the EoS parameter [Formula: see text], all models give evidence of their candidature for the explanation of the phantom regime and also the quintessence regime in the late stage of the universe. Also, the stability condition ensures that our reconstructed models are classically stable.

Reconstructions of f(P) gravity from (m,n) type ordinary and entropy-corrected holographic and Pilgrim dark energy models

Modified gravity models are popular among cosmologists, as they can describe the cosmological evolution quite efficiently. Reconstruction of newly introduced [Formula: see text] gravity, with the help of ordinary, power-law entropy corrected and logarithmic entropy-corrected versions of Holographic dark energy (HDE) and Pilgrim dark energy (PDE) models have been studied in this work. For such reconstruction, we have considered the power-law scale factor [Formula: see text]. Further, the classical stabilities (the squared speed of sound method) of such reconstructions and their implications on the nature of the equation of state (EoS) parameters and deceleration parameter with respect to red-shift have also been examined. Finally, we have computed the age of the universe for reconstructed models.

Nature of Higher-Dimensional Wormhole Mass Due to Accretion of Entropy Corrected Holographic and New Agegraphic Dark Energies

We study the accretion of dark matter and dark energy onto $$(n+2)$$ -dimensional Morris–Thorne wormholes. The wormhole mass and its rate of change have been written in the background of the $$(n+2)$$ -dimensional Friedmann-Robertson-Walker (FRW) model of the Universe. We have assumed the candidates of dark energy in the form of entropy-corrected holographic dark energy (ECHDE) and entropy-corrected new agegraphic dark energy (ECNADE) with its logarithmic and power-law versions. For these different dark energy models, the wormhole mass has been calculated in terms of the redshift when dark matter and the above types of dark energies accrete onto the wormhole. For this purpose, we have taken two classes of scale factors, where in class I the scale factor describes a future singularity while class II follows from an initial singularity. We graphically present the nature of the wormhole mass in different dimensions (4D, 5D, 6D) for ECHDE and ECNADE accretion. In the class I scale factor, we observe that the wormhole mass increases during the evolution of the Universe in both ECHDE and ECNADE models in both the power-law and logarithmic versions. Also, with the class II scale factor, we see that the wormhole mass decreases during the evolution of the Universe for ECHDE in both power-law and logarithmic versions, and for ECNADE with power law models, while the wormhole mass increases during the evolution of the Universe for ECNADE in its logarithmic version.

A stable flat entropy-corrected FRW universe

In this paper, a general entropy-corrected FRW cosmological model has been presented in which a deceleration-to-acceleration transition occurs according to recent observations. We found that the case for the flat universe ([Formula: see text]), supported by observations, is the most stable one where it successfully passes all stability tests. The stability of the model has been studied through testing the sound speed, the classical and the new nonlinear energy conditions. The model predicts a positive pressure during the early-time decelerating epoch, and a negative pressure during the late-time accelerating epoch in a good agreement with cosmic history and dark energy assumption. We have investigated all possible values of the prefactors [Formula: see text] and [Formula: see text] in the corrected entropy-area relation to find the best values required for a stable flat universe. We have also made use of the evolution of the equation of state parameters [Formula: see text] in predicting the correct values of [Formula: see text] and [Formula: see text]. The jerk and density parameters have been calculated where a good agreement with observations and [Formula: see text]CDM model has been obtained. Two dark energy proposals have been investigated in this model, the entropy-corrected holographic dark energy and the modified holographic Ricci dark energy.

Holographic dark energy models with interactions and entropy corrections for different cutoffs in the Brans–Dicke cosmology

In the framework of Brans-Dicke cosmology, we have studied the interacting power-law and logarithmic entropy-corrected holographic dark energy models with different cut-offs. The Brans-Dicke parameter is investigated versus the conditions for the acceleration and phantom phases to show that which entropy corrected model can exhibit acceleration with or without the phantom phase at early and present time universes. Moreover, the classical stability or instability of the interacting power-law and logarithmic entropy-corrected holographic dark energy models with different cut-offs is determined at early and present time

Inflation via logarithmic entropy-corrected holographic dark energy model

We study the inflation via logarithmic entropy-corrected holographic dark energy LECHDE model with future event horizon, particle horizon and Hubble horizon cut-offs, and compare the results with those of obtained in the study of inflation by holographic dark energy HDE model. In comparison, the spectrum of primordial scalar power spectrum in the LECHDE model becomes redder than the spectrum in HDE model. Moreover, the consistency with the observational data in LECHDE model of inflation, constrains the reheating temperature and Hubble parameter by one parameter of holographic dark energy and two new parameters of logarithmic corrections.

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

In this paper, we study the Power-Law Entropy-Corrected Holographic Dark Energy (PLECHDE) model in the framework of Hořava-Lifshitz cosmology considering a non-flat Universe. As infrared cut-off of the system, we choose the recently proposed Granda-Oliveros (GO) cut-off, which is a function of the Hubble parameter squared H2 and of the first time derivative of the Hubble parameter $\dot{H}$ . Moreover, the GO cut-off is characterized by two constant parameters, $\alpha$ and $\beta$ , representing the multiplying factors of the two terms forming the cut-off itself. We derive the evolutionary form of the fractional energy densities of DE, DM and curvature $\Omega_{D}'$ , $\Omega_{m}'$ and $\Omega_{k}'$ , the pressure of DE pD, the Equation-of-State (EoS) parameter of DE $\omega_{D}$ and the deceleration parameter q . Using the parametrization of the EoS parameter $\omega_{D}(z) = \omega_{0}+\omega_{1} z$ , we obtain the expressions of $\omega_{0}$ and $\omega_{1}$ . We also study the behavior of the statefinder parameters {r,s}, the snap and lerk cosmographic parameters $s_{cosmo}$ and l and the squared speed of the sound v s 2 in order to have a better comprehension of the properties of the model considered. We also calculate the present day values of the quantities we study for different values of the running parameter $\lambda$ (which is a characteristic parameter of Hořava-Lifshitz cosmology) and for different sets of values of $\alpha$ and $\beta$ . All the quantities are derived for both non-interacting and interacting DE and Dark Matter (DM).

Reconstructions of f(T) gravity from entropy-corrected holographic and new agegraphic dark energy models in power-law and logarithmic versions

Here, we peruse cosmological usage of the most promising candidates of dark energy in the framework of $f(T)$ gravity theory. We reconstruct the different $f(T)$ modifed gravity models in the spatially flat FRW universe according to entropy-corrected versions of the holographic and new agegraphic dark energy models in power-law and logarithmic corrections, which describe accelerated expansion history of the universe. We conclude that the equation of state parameter of the entropy-corrected models can transit from quintessence state to phantom regime as indicated by recent observations or can lie entirely in the phantom region. Also, using these models, we investigate the different erase of the stability with the help of the squared speed of sound.

Power-law entropy-corrected new holographic dark energy in Brans–Dicke cosmology

The purpose of this paper is to study power-law entropy-corrected holographic dark energy (PLECHDE) in the framework of Brans–Dicke cosmology with Granda–Oliveros (G-O) IR-cutoff. Considering the interacting and non-interacting scenario of PLECHDE with dark matter, we investigate the cosmological implications of this model in detail. We obtain the equation of state parameter, deceleration parameter, and evolution of dark energy density to explain expansion of the universe. We also determine these parameters for Ricci scale. We extend our study of the power-law entropy-corrected agegraphic dark energy model and calculate some cosmological parameters. Further, we show that the results that we calculate have good compatibility with previous work and matches it in the limiting case. Finally, we find a cosmological application of our work by evaluating the equation of state of dark energy for low red-shift.

Reconstructing f(R), f(G), f(T), and Einstein-Aether gravities from entropy-corrected (m,n) type pilgrim dark energy

First, we describe the ordinary holographic dark energy (HDE), (m,n) type holographic dark energy, entropy-corrected holographic dark energy (ECHDE) for logarithmic and power-law versions and pilgrim dark energy (PDE) models. Next, we introduce the (m,n) type pilgrim dark energy and its entropy-corrected versions of logarithmic and power-law forms i.e., (m,n) type LECPDE and PLECPDE models. The main motivation of the work is to have reconstructions of f(R), f(G), f(T), and Einstein-Aether gravities from (m,n) type entropy-corrected pilgrim dark energy (ECPDE). Briefly the idea of our proposed entropy-corrected (m,n) type pilgrim dark energy model is discussed. We also discuss the modified Friedmann equations for f(R), f(G), f(T), and Einstein-Aether gravities and then from the equations we find the effective density and pressure for the f(R), f(G), f(T), and Einstein-Aether gravities sectors, respectively. These can be treated as an effective dark energy. Assuming the power-law solution of the scale factor, a∼tδ, we can reconstruct the unknown functions of f(R), f(G), f(T), and F(K) of Einstein-Aether gravities from logarithmic and power-law corrected versions of ECPDE. Finally, we give some cosmological implications of the reconstructed models.

Power-law entropy-corrected new holographic dark energy in Horava–Lifshitz cosmology

Purpose of this paper is to study power-law entropy-corrected holographic dark energy (PLECHDE) in the frame work of Horava–Lifshitz cosmology with Granda–Oliveros (G-O) IR-cutoff. Considering interacting and non-interacting scenario of PLECHDE with dark matter in a spatially non-flat universe, we investigate the cosmological implications of this model in detail. We obtain equation of state parameter, deceleration parameter and the evolution of dark energy density to explain the expansion of the universe. We also find out these parameters for Ricci scale. Finally, we find out a cosmological application of our work by evaluating a relation for the equation of state of dark energy for law red-shifts.

ENTROPY CORRECTED HOLOGRAPHIC DARK ENERGY f(T) GRAVITY MODEL

This paper is devoted to study the power-law entropy corrected holographic dark energy (ECHDE) model in the framework of f(T) gravity. We assume infrared (IR) cutoff in terms of Granda–Oliveros (GO) length and discuss the constructed f(T) model in interacting as well as in non-interacting scenarios. We explore some cosmological parameters like equation of state (EoS), deceleration, statefinder parameters as well as ωT–ωT′ analysis. The EoS and deceleration parameters indicate phantom behavior of the accelerated expansion of the universe. It is mentioned here that statefinder trajectories represent consistent results with ΛCDM limit, while evolution trajectory of ωT–ωT′ phase plane does not approach to ΛCDM limit for both interacting and non-interacting cases.

Interacting Entropy-Corrected Holographic Dark Energy and IR Cut-Off Length

In this paper we consider holographic dark energy model with corrected holographic energy density and show that this model may be equivalent to the modified Chaplygin gas model. Then we obtain relation between entropy corrected holographic dark energy model and scalar field models. We do these works by using choices of IR cut-off length proportional to the Hubble radius, the event horizon radius, the Ricci length, and the Granda-Oliveros length.

Logarithmic Entropy-Corrected Holographic Dark Energy in Hořava-Lifshitz cosmology with Granda-Oliveros cut-off

In this work, we studied the Logarithmic Entropy-Corrected Holographic Dark Energy (LECHDE) model in a spatially non-flat universe and in the framework of Hořava-Lifshitz cosmology. As infrared cutoff of the system we considered the cut-off recently proposed by Granda and Oliveros which contains two terms, one proportional to H 2 and one to \(\dot{H}\). For the two cases containing non-interacting and interacting Dark Energy (DE) and Dark Matter (DM), we obtained the exact differential equation that determines the evolution of the density parameter. Moreover, we derived the expressions of the deceleration parameter q and, using a parametrization of the equation of state (EoS) parameter ω D of our model as ω D (z)=ω 0+ω 1 z, we derived both the expressions of ω 0 and ω 1 for both non-interacting and interacting cases. All derivations made in this work are done in small redshift approximation and for low redshift expansion of the equation of state (EoS) parameter.

Interacting Ricci Logarithmic Entropy-Corrected Holographic Dark Energy in Brans-Dicke Cosmology

In the derivation of Holographic Dark Energy (HDE), the area law of the black hole entropy assumes a crucial role. However, the entropy-area relation can be modified including some quantum effects, motivated from the Loop Quantum Gravity (LQG), string theory and black hole physics. In this paper, we study the cosmological implications of the interacting logarithmic entropy-corrected HDE (LECHDE) model in the framework of Brans-Dicke (BD) cosmology. As system’s infrared (IR) cut-off, we choose the average radius of Ricci scalar curvature, i.e. R −1/2. We obtain the Equation of State (EoS) parameter ω D , the deceleration parameter q and the evolution of energy density parameter $\varOmega'_{D}$ of our model in a non-flat universe. Moreover, we study the limiting cases corresponding to our model without corrections and to the Einstein’s gravity.

The entropy-corrected holographic dark energy in Brans-Dicke cosmology with varying mass fermions

We aim in this paper to study Brans-Dicke cosmology in the presence of varying mass fermions and a self-interaction potential. Furthermore, we also probe the entropy corrected holographic dark energy (ECHDE) in the model in two non-interacting and interacting scenarios. The model parameters are constrained by using the recent SNe Ia observational data and tested against observational data of Hubble parameter. For a comparison, we also constrained and tested the cosmological parameters in ΛCDM model with the same observational data. We show that in non of the scenarios the model prediction is better than ΛCDM model.

F(G) gravity models based on the ordinary and entropy-corrected holographic dark energy models

The ordinary and entropy-corrected versions of the holographic dark energy models in the spatially flat Friedmann–Robertson–Walker universe are considered. Then the F(G) modified gravity models as a candidates of dark energy are reconstructed according to the ordinary and entropy-corrected versions of the holographic dark energy models. The EoS parameters corresponding to the F(G) gravity models are obtained. The validity phantom or quintessence models in this framework of the modified gravity are investigated.

Interacting Ricci dark energy with logarithmic correction

Motivated by the holographic principle, it has been suggested that the dark energy density may be inversely proportional to the area $A$ of the event horizon of the universe. However, such a model would have a causality problem. In this work, we consider the entropy-corrected version of the holographic dark energy model in the non-flat FRW universe and we propose to replace the future event horizon area with the inverse of the Ricci scalar curvature. We obtain the equation of state (EoS) parameter $\omega_{\Lambda}$, the deceleration parameter $q$ and $\Omega_D'$ in the presence of interaction between Dark Energy (DE) and Dark Matter (DM). Moreover, we reconstruct the potential and the dynamics of the tachyon, K-essence, dilaton and quintessence scalar field models according to the evolutionary behavior of the interacting entropy-corrected holographic dark energy model.

Interacting entropy-corrected holographic dark energy with apparent horizon as an infrared cutoff

In this work we consider the entropy-corrected version of interacting holographic dark energy (HDE), in the non-flat universe enclosed by apparent horizon. Two corrections of entropy so-called logarithmic ‘LEC’ and power-law ‘PLEC’ in HDE model with apparent horizon as an IR-cutoff are studied. The ratio of dark matter to dark energy densities u, equation of state parameter w D and deceleration parameter q are obtained. We show that the cosmic coincidence problem is solved for interacting models. By studying the effect of interaction in EoS parameter of both models, we see that the phantom divide may be crossed and also understand that the interacting models can drive an acceleration expansion at the present and future, while in non-interacting case, this expansion can happen only at the early time. The graphs of deceleration parameter for interacting models, show that the present acceleration expansion is preceded by a sufficiently long period deceleration at past. Moreover, the thermodynamical interpretation of interaction between LECHDE and dark matter is described. We obtain a relation between the interaction term of dark components and thermal fluctuation in a non-flat universe, bounded by the apparent horizon. In limiting case, for ordinary HDE, the relation of interaction term versus thermal fluctuation is also calculated.

Interacting viscous entropy-corrected holographic scalar field models of dark energy with time-varying G in modified FRW cosmology

We study the entropy-corrected version of the holographic dark energy (HDE) model in the framework of modified Friedmann-Robertson-Walker cosmology. We consider a non-flat universe filled with an interacting viscous entropy-corrected HDE (ECHDE) with dark matter. Also included in our model is the case of the variable gravitational constant G. We obtain the equation of state and the deceleration parameters of the interacting viscous ECHDE. Moreover, we reconstruct the potential and the dynamics of the quintessence, tachyon, K-essence and dilaton scalar field models according to the evolutionary behavior of the interacting viscous ECHDE model with time-varying G.