Anisotropic Cosmological Models with Quintessence

Kotambkar, S.; Singh, G. P.; Kelkar, R.

doi:10.1007/s10773-013-1829-3

Cited by 15 publications

(6 citation statements)

References 42 publications

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“…The mean Hubble parameter and deceleration parameter respectively are given as H = n t and q = −1 + 1 n . Using the observational value for q = −0.33 ± 0.17 [49], we have restricted n as n ∈ (1.19, 2) in case of polynomial law model. The scalar expansion and shear scalar are obtained as θ = 3n t and σ 2 = l 2 1 3t 6n respectively.…”

Section: Power Law Volume Expansion Modelmentioning

confidence: 99%

Scalar field and time varying cosmological constant in f ( R , T ) gravity for Bianchi type-I universe

Singh

Bishi

Sahoo

2016

Chinese Journal of Physics

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In this article, we have analysed the behaviour of scalar field and cosmological constant in f (R, T ) theory of gravity. Here, we have considered the simplest form of f (R, T ) i.e. f (R, T ) = R + 2f (T ), where R is the Ricci scalar and T is the trace of the energy momentum tensor and explored the spatially homogeneous and anisotropic Locally Rotationally Symmetric (LRS) Bianchi type-I cosmological model. It is assumed that the Universe is filled with two non-interacting matter sources namely scalar field (normal or phantom) with scalar potential and matter contribution due to f (R, T ) action. We have discussed two cosmological models according to power law and exponential law of the volume expansion along with constant and exponential scalar potential as sub models. Power law models are compatible with normal (quintessence) and phantom scalar field whereas exponential volume expansion models are compatible with only normal (quintessence) scalar field. The values of cosmological constant in our models are in agreement with the observational results. Finally, we have discussed some physical and kinematical properties of both the models.

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Section: Power Law Volume Expansion Modelmentioning

confidence: 99%

Scalar field and time varying cosmological constant in f ( R , T ) gravity for Bianchi type-I universe

Singh

Bishi

Sahoo

2016

Chinese Journal of Physics

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“…The directional Hubble parameters are obtained as H i = n t + Xoi V0t 3n , i = 1, 2, 3. The Hubble parameter (H), deceleration parameter (q) , expansion scalar (Θ) and Shear scalar (σ 2 ) are as follows H = n t , q = −1 + 1 n , Θ = 3 n t , σ 2 = X 2 02 + X 2 03 + X 02 X 03 V 2 0 t 6n Using the observational value for q = −0.33 ± 0.17 [37], we have restricted n as n ∈ (1.19, 2) in case of Power law model. Here we noticed that H,Θ and σ 2 die out for larger values of t. With the help of (27) from (26), the energy density is obtained as…”

Section: Power Law Modelmentioning

confidence: 99%

Bianchi Type-I Universe with Cosmological Constant and Quadratic Equation of State inf(R,T)Modified Gravity

Singh

Bishi

2015

Advances in High Energy Physics

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This article deals with the study of Bianchi type-I universe in the context of f (R, T ) gravity. Einstein's field equations in f (R, T ) gravity has been solved in presence of cosmological constant Λ and quadratic equation of state (EoS) p = αρ 2 − ρ, where α = 0 is a constant. Here we have discussed two classes of f (R, T ) gravity i.e. f (R, T ) = R + 2f (T ) and f (R, T ) = f1(R) + f2(T ). A set of models has been taken into consideration based on the plausible relation. Also we have studied the some physical and kinematical properties of the models.

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“…Naidu et al examined spatially homogeneous and anisotropic Bianchi type II [55] and III [56] models based on Saez and Ballester theory. Based on the same theory, the authors also investigated Bianchi type V [57] model with variable ω and constant q. Kotambkar et al [58] constructed anisotropic Bianchi type I model with bulk viscosity and quintessence and discussed various physical properties of the model. Singh et al [59] examined Bianchi type II model for a perfect fluid source in f (R, T ) gravity.…”

Section: Introductionmentioning

confidence: 99%

Mixed fluid cosmological model in $f(R,T)$ gravity

Sahoo,

Taori,

Mahanta

2020

Preprint

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We construct Locally Rotationally Symmetric (LRS) Bianchi type-I cosmological model in f (R, T ) theory of gravity when the source of gravitation is the mixture of barotropic fluid and dark energy (DE) by employing a time varying deceleration parameter (DP). We observe through the behavior of the state finder parameters (r, s) that our model begins from the Einstein static era and goes to ΛCDM era. The EoS parameter(ω d ) for DE varies from phantom (ω < −1) phase to quintessence (ω > −1) phase which is consistent with the observational results. It is found that the discussed model can reproduce the current accelerating phase of expansion of the universe.

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Anisotropic Cosmological Models with Quintessence

Cited by 15 publications

References 42 publications

Scalar field and time varying cosmological constant in f ( R , T ) gravity for Bianchi type-I universe

Scalar field and time varying cosmological constant in f ( R , T ) gravity for Bianchi type-I universe

Bianchi Type-I Universe with Cosmological Constant and Quadratic Equation of State inf(R,T)Modified Gravity

Mixed fluid cosmological model in $f(R,T)$ gravity

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