Panorama Behaviors of Holographic Dark Energy Models in Modified Gravity

Shaikh, A. Y.; Wankhade, K. S.

doi:10.1007/s10701-021-00463-8

Cited by 6 publications

(3 citation statements)

References 79 publications

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“…Here, this work employs the time-varying deceleration parameter suggested by Dewri (1) which shows a sign-flipping property from early-time deceleration to late-time acceleration. The model starts to expand from an initial Big Bang singularity at t = 0.25 with zero volume to de-sitter expansion at t → ∞ in which q = −1 and dH dt = 0, which matches the result of Shaikh and Wankhade's (22) . The evolution of energy density shows a positively decreasing function of time, and the pressure is always negative, which approaches zero at late times.…”

Section: Discussionsupporting

confidence: 70%

“…Therefore, the deceleration parameter in this study has a sign-flipping property depending on time ′ t ′ , as represented in Figure 3 (a). In Shaikh and Wankhade's (22) study of f (R, T ) gravity, the same sign-flipping deceleration parameter independent of time 't' was also noted for LRS Bianchi type-I. Also, from Equation (27), it is observed that the present value of the deceleration parameter at t 0 = 13.8 Gigayear (Gyr), is q 0 (t) = −0.730 and at t → ∞, it tends to de-sitter expansion https://www.indjst.org/ (q = −1).…”

Section: Resultsmentioning

confidence: 99%

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Dynamics of Bianchi Type-III Universe with Time-Varying Deceleration Parameter in f (G) Gravity

Basumatary,

Dewri

2023

IJST

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Objectives: To explore Bianchi type-III cosmological models in f (G) gravity theory with time-varying deceleration parameters. Methods: In this paper, to get the exact solution of the field equation in the presence of perfect fluid, we consider: (i) the relation that shear scalar (σ )is proportional to the expansion scalar(θ ), resulting in C = B n . (ii) time-varying deceleration parameter, q = −1 + 1 √ t suggested by Dewri (1) , indicating an accelerated expansion of the universe. (iii) the power-law f (G) model, which is compatible with the recent observational data. Also, along with the graphical representation, the geometrical and physical aspects are examined. Findings: In this study, the model transit from the early decelerating phase(q > 0) to the present accelerating phase (q < 0), and in support of that, violation of the strong energy condition with negative pressure is observed, ultimately indicating the presence of the dark energy. It is worthwhile to mention that the contribution of dark energy initially lies in the phantom domain(ω < −1). After a period of time, it extends to the quintessence domain(ω > −1) and later approaches to Λ cold dark matter (CDM) model (ω = −1) at a late time. Novelty: The universe's evolution has been explored in the framework of f (G) gravity, identifying the cosmological parameters of the model obtained in this work. The negative pressure and the falling of strong energy conditions suggest its consistency with the recent cosmological observation of the dark energy universe, and the findings of this study may contribute to a deeper comprehension of the universe's accelerated expansion.

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Section: Discussionsupporting

confidence: 70%

Section: Resultsmentioning

confidence: 99%

Dynamics of Bianchi Type-III Universe with Time-Varying Deceleration Parameter in f (G) Gravity

Basumatary,

Dewri

2023

IJST

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“…Sarma [28] studied THDE in f (R, T) theory using the axially symmetric Bianchi-I space time in a recent paper. By studying volumetric power and exponential laws, Shaikh and Wankhade [29] discovered solutions in f (R, T) theory with Bianchi I Kasner form spacetime. In a different study, Varshney et al [30] looked at the equivalence of the scalar fields of tachyon, phantom, and Dirac Born-Infeld-essence with THDE in the context of f (R, T) gravity.…”

Section: Introductionmentioning

confidence: 99%

Statefinder diagnosis of Tsallis holographic dark energy model in f(R, T) Theory

Memet¹,

Aktaş²

2022

Phys. Scr.

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In this study, Tsallis Holographic Dark Energy (THDE) was studied in the framework of $f(R, T)$ gravitational theory by taking into consideration the homogeneous and anisotropic Bianchi-I spacetime. The Hubble horizon was chosen as $IR$ cutoff of the system. To obtain solutions of field equations, THDE density and a form of Hubble parameter were used. Additionally, various physical parameters such as energy of state parameter, deceleration parameter and scale factor have been discussed. The characteristics and parameters of the model have been also examined by plotting their evolution graphics. Furthermore, statefinder parameters, which are effective tools for separating dark energy models, have been explored. By the illustration of trajectory in $r-s$ plane, it is found that this model behaves like Chaplygin gas at initial stage, then ranging in quintessence region it finally approaches to $\Lambda$ Cold Dark Matter. Lastly, from the evolutions of $r-q$ and $s-q$ planes it is seen that the model evolves to the De Sitter expansion point.

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Bianchi type-III holographic dark energy cosmological model in f(R,T) theory of gravitation

Mule

Gaikwad²,

Mete

2024

New Astronomy

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Panorama Behaviors of Holographic Dark Energy Models in Modified Gravity

Cited by 6 publications

References 79 publications

Dynamics of Bianchi Type-III Universe with Time-Varying Deceleration Parameter in f (G) Gravity

Dynamics of Bianchi Type-III Universe with Time-Varying Deceleration Parameter in f (G) Gravity

Statefinder diagnosis of Tsallis holographic dark energy model in f(R, T) Theory

Bianchi type-III holographic dark energy cosmological model in f(R,T) theory of gravitation

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