Some anisotropic dark energy models in Bianchi type-V space-time

Yadav, Anil Kumar

doi:10.1007/s10509-011-0745-3

Cited by 101 publications

(55 citation statements)

References 34 publications

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“…We notice that, in connection to anisotropic equation of state for dark energy, several works are now available in the literature [29,30,31]. Some Authors [32,33,34,35,36,37,38] have studied anisotropic DE models even with constant deceleration parameter (DP).…”

Section: Introductionmentioning

confidence: 99%

Magnetized dark energy and the late time acceleration

Yadav

Rahaman

Ray³

et al. 2012

Eur. Phys. J. Plus

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In the present work we have searched the existence of the late time acceleration of the Universe. The matter source that is responsible for the late time acceleration of the Universe consists of cosmic fluid with the equation of state parameter ω = p/ρ and uniform magnetic field of energy density ρ B . The study is done here under the framework of spatially homogeneous and anisotropic locally rotationally symmetric (LRS) Bianchi-I cosmological model in the presence of magnetized dark energy. To get the deterministic model of the Universe, we assume that the shear scalar (σ) in the model is proportional to expansion scalar (θ). This condition leads to A = B n , where A and B are metric functions and n is a positive constant giving the proportionality condition between shear and expansion scalar. It has been found that the isotropic distribution of magnetized dark energy leads to the present accelerated expansion of the Universe and the derived model is in good agreement with the recent astrophysical observations. The physical behavior of the Universe has been discussed in details.

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Section: Introductionmentioning

confidence: 99%

Magnetized dark energy and the late time acceleration

Yadav

Rahaman

Ray³

et al. 2012

Eur. Phys. J. Plus

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“…This ansatz generalized the one proposed by Amirhashchi et al [52]. In literature it is common to use a constant deceleration parameter [37,38,41,53,21,22] as it duly gives a power law for metric function or corresponding quantity. The motivation to choose such time dependent DP is behind the fact that the universe is accelerated expansion at present as observed in recent observations of Type Ia supernova [1]− [4] and CMB anisotropies [54]− [56] and decelerated expansion in the past.…”

Section: Solution Of the Field Equations And Its Physical Significancementioning

confidence: 82%

“…[22]. Yadav [21] and Kumar & Yadav [22] have solved the field equations by considering the constant DP whereas we have considered time dependent DP. As we have already discussed in previous Sect.…”

Section: Discussion and Concluding Remarksmentioning

confidence: 99%

“…Following, Akarsu and Kilinc [37,38,50] and Yadav [21], we split the conservation of energy momentum tensor of the DE into two parts, one corresponds to deviations of EoS parameter and other is the deviation-free part of T (de)ij ;j = 0:…”

Section: Solution Of the Field Equations And Its Physical Significancementioning

confidence: 99%

“…Thus, the Bianchi type-V models which remain anisotropic are of rather academic interest. Recently, Yadav [21] and Kumar & Yadav [22] have dealed with a spatially homogeneous and anisotropic Bianchi type-V DE models by considering constant deceleration parameter.…”

Section: Introductionmentioning

confidence: 99%

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Accelerating Dark Energy Models in Bianchi Type-v Spacetime

Pradhan

Amirhashchi

2011

Mod. Phys. Lett. A

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Some new exact solutions of Einstein's field equations have emerged in a spatially homogeneous and anisotropic Bianchi type-V space-time with minimally interacting perfect fluid and anisotropic dark energy (DE) components, which has dynamic equation of state (EoS). We consider Bianchi type-V space-time, introducing three different skewness parameters along spatial directions to quantify deviation of pressure from isotropy. To obtain the deterministic solution we choose the scale factor a(t) = √ t n e t , which yields a time-dependent deceleration parameter (DP). We find that the time dependent value of deceleration parameter is reasonable for the present day universe which yields a transition of the universe from the early decelerating phase to the recent accelerating phase. For different values of n, we can generate a class of physically viable DE models. It is found that quintessence model is suitable for describing the present evolution of the universe. The physical and geometric properties of spatially homogeneous and anisotropic cosmological models are discussed.

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Modeling of Accelerating Universe with Bulk Viscous Fluid in Bianchi V Space‐Time

Goswami

Yadav²,

Mishra

et al. 2021

Fortschritte der Physik

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In this paper, we have investigated a bulk viscous anisotropic Universe and constrained its model parameters with recent H(z) and Pantheon compilation data. Using cosmic chronometric technique, we estimate the present value of Hubble's constant as H0=69.39±1.54kms−1Mpc−1, 70.016±1.65kms−1Mpc−1 and 69.36±1.42kms−1Mpc−1 by bounding our derived model with recent H(z) data, Pantheon and joint H(z) and Pantheon data respectively. The present age of the Universe is specified as t0=0.9796H0−1∼13.79 Gyrs. The model favours a transitioning Universe with the transition red‐shift as zt=0.73. We have reconstructed the jerk parameter using the observational data sets. From the analysis of the jerk parameter, it is observed that, our derived model shows a marginal departure from the concordance ΛCDM model.

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Some anisotropic dark energy models in Bianchi type-V space-time

Cited by 101 publications

References 34 publications

Magnetized dark energy and the late time acceleration

Magnetized dark energy and the late time acceleration

Accelerating Dark Energy Models in Bianchi Type-v Spacetime

Modeling of Accelerating Universe with Bulk Viscous Fluid in Bianchi V Space‐Time

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