Dark energy models with anisotropic fluid in Bianchi Type-VI 0 space-time with time dependent deceleration parameter

Pradhan, Anirudh; Jaiswal, Rekha; Jotania, Kanti; Khare, R. K.

doi:10.1007/s10509-011-0835-2

Cited by 69 publications

(24 citation statements)

References 124 publications

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“…The derivation and the motivation to choose such scale factor has already been described in details by Pradhan [62]. This relation (42) generalizes the value of scale factor obtained by Pradhan et al [65,66] Eqs. (39)−(41) with the help of (42), we obtain the metric functions as (17), we obtain obtain the expressions for pressure (p), energy density (ρ) and cosmological constant (Λ) for the model (18) as…”

Section: The Basic Equations and Quadrature Solutionssupporting

confidence: 62%

V cosmological models in f(R,T) modified gravity with Λ(T) by using generation technique

Ahmed

Pradhan

Fekry

et al. 2016

NRIAG Journal of Astronomy and Geophysics

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A new class of cosmological models in f (R, T ) modified theories of gravity proposed by Harko et al. (2011), has been investigated for a specific choice of f (R, T ) = f1(R) + f2(T ) by considering time dependent deceleration parameter. The concept of time dependent deceleration parameter (DP) with some proper assumptions yield the average scale factor a(t) = sinh 1 n (αt), where n and α are positive constants. For 0 < n ≤ 1, this generates a class of accelerating models while for n > 1, the models of universe exhibit phase transition from early decelerating phase to present accelerating phase which is in good agreement with the results from recent astrophysical observations. Our intention is to reconstruct f (R, T ) models inspired by this special law for the deceleration parameter in connection with the theories of modified gravity. In the present study we consider the cosmological constant Λ as a function of the trace of the stress energymomentum-tensor, and dub such a model "Λ(T ) gravity" where we have specified a certain form of Λ(T ). Such models may display better uniformity with the cosmological observations. The statefinder diagnostic pair {r, s} parameter has been embraced to characterize different phases of the universe. We also discuss the physical consequences of the derived models.

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Section: The Basic Equations and Quadrature Solutionssupporting

confidence: 62%

V cosmological models in f(R,T) modified gravity with Λ(T) by using generation technique

Ahmed

Pradhan

Fekry

et al. 2016

NRIAG Journal of Astronomy and Geophysics

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“…(69), we note that energy density of the fluid ρ(t) is a decreasing function of time and ρ > 0 under condition (82) This behaviour of energy density ρ(t) is clearly shown in Fig. 5 in the two modes of the evolution of the uni verse.…”

Section: Bianchi Type II Anisotropicmentioning

confidence: 66%

“…Setare [64][65][66] and Setare and Saridakis [67][68][69] have also studied the DE models in different contexts. Recently, dark energy models with variable EoS parameter have been studied by Ray et al [70], Akarsu and Kilinc [71][72][73][74], Yadav et al [75], Yadav and Yadav [76], Yadav and Saha [77] Pradhan and Amirhashchi [78,79], Pradhan et al [80][81][82], Amirhashchi et al [83][84][85][86], Kumar [87,88], Kumar and Akarsu [89], Kumar and Yadav [90] and Kumar and Singh [91]. In well known reviews on modified gravity [92,93], it is clearly indicated that any modified gravity may be represented as effective fluid with time dependent ω.…”

Section: Introductionmentioning

confidence: 99%

Accelerating dark energy models of the universe in anisotropic Bianchi type space-times and recent observations

Pradhan

Saha

2015

Phys. Part. Nuclei

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Motivated by the increasing evidence for the need of a geometry that resembles Bianchi morphol ogy to explain the observed anisotropy in the WMAP data, we have discussed some features of the Bianchi type universes in the presence of a fluid that wields an anisotropic equation of state (EoS) parameter in gen eral relativity. Such models are of great interest in cosmology in favor of constructing more realistic models than FLRW models with maximally symmetric spatial geometry. Additionally, the interest in such models was promoted in recent years due to the debate that going on the analysis and the interpretation of the WMAP [21,111,112] data, whether they need a Bianchi type morphology to be explained successfully [7,103,118,117]. The LLC-WMAP data maps show seven axes well aligned with one another and the direction Virgo. For this reason Bianchi models are important in the study of anisotropies. In the present study of Bianchi type I, II, III, V and VI 0 space times, we observe that the EoS for dark energy ω is found to be time dependent and its existing range for derived models is in good agreement with the recent observations of SNe Ia data [50], SNe Ia data with CMBR anisotropy and galaxy clustering statistics [11] and latest combination of cosmological datasets coming from CMB anisotropies, luminosity distances of high redshift type Ia supernovae and galaxy clustering [21,51]. It has been suggested that the dark energy that explains the observed accelerating expan sion of the universe may arise due to the contribution to the vacuum energy of the EoS in a time dependent background. The cosmological constant Λ is found to be a positive decreasing function of time and it approaches to a small positive value at late time (i.e. the present epoch) which is corroborated by results from recent type Ia supernovae observations.

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“…We consider the deceleration parameter to be a variable ( ) and following Pradhan et al [65] and Chawla et al [1], we assume the law of variation of scale factor as increasing function of time…”

Section: Cosmological Solution For Variable Deceleration Parametermentioning

confidence: 99%

Interacting Holographic Dark Energy in Bianchi Type-V Universe with Variable Deceleration Parameter

Mete¹,

Bokey²,

Bawane³

2019

OALib

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Dark energy models with anisotropic fluid in Bianchi Type-VI 0 space-time with time dependent deceleration parameter

Cited by 69 publications

References 124 publications

V cosmological models in f(R,T) modified gravity with Λ(T) by using generation technique

V cosmological models in f(R,T) modified gravity with Λ(T) by using generation technique

Accelerating dark energy models of the universe in anisotropic Bianchi type space-times and recent observations

Interacting Holographic Dark Energy in Bianchi Type-V Universe with Variable Deceleration Parameter

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