Power-Law Expansion and Scalar Field Cosmology in Higher Derivative Theory

Singh, C. P.; Singh, Vijay

doi:10.1007/s10773-011-1065-7

Cited by 8 publications

(6 citation statements)

References 32 publications

(32 reference statements)

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“…In other words, the energy density of matter must be positive. This procedure has been followed in many earlier works [67,68,69,70,71,72,73,74,75] (see also our recent work [66] and references therein).…”

Section: The Model In Einstein's Gravitymentioning

confidence: 99%

Plane symmetric model in f(R, T) gravity

Singh

Беешам

2020

Eur. Phys. J. Plus

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A plane symmetric Bianchi-I model is explored in f (R, T ) gravity, where R is the Ricci scalar and T is the trace of energy-momentum tensor. The solutions are obtained with the consideration of a specific Hubble parameter which yields a constant deceleration parameter. The various evolutionary phases are identified under the constraints obtained for physically viable cosmological scenarios. Although a single (primary) matter source is taken, due to the coupling between matter and f (R, T ) gravity, an additional matter source appears, which mimics a perfect fluid or exotic matter. The solutions are also extended to the case of a scalar field model. The kinematical behavior of the model remains independent of f (R, T ) gravity. The physical behavior of the effective matter also remains the same as in general relativity. It is found that f (R, T ) gravity can be a good alternative to the hypothetical candidates of dark energy to describe the present accelerating expansion of the universe.

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Section: The Model In Einstein's Gravitymentioning

confidence: 99%

Plane symmetric model in f(R, T) gravity

Singh

Беешам

2020

Eur. Phys. J. Plus

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“…Harko et al [70] have presented several exact cosmological solutions with a scalar field as the only matter source in GR. Many researchers have studied some of the most intriguing aspects of our universe containing a self-interacting scalar field possessing an interaction potential as the only matter source in modified gravity [69,71,72]. In [52], the authors also have introduced a version of f (R, T ) gravity for scalar field cosmology, namely, f (R, T φ ) gravity by considering in the action an algebraic function F(R, φ) of the Ricci curvature R and scalar field φ.…”

Section: The Model and Field Equations In F (R T φ ) Gravitymentioning

confidence: 99%

The $$f(R,T^\phi )$$ f ( R , T ϕ ) gravity models with conservation of energy–momentum tensor

Singh

Беешам

2018

Eur. Phys. J. C

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In this paper, we have derived a spatially flat homogeneous and isotropic cosmological model in f (R, T φ ) gravity with a scalar field. In addition to a minimally coupled scalar field with self interacting potential, we also have a contribution from the coupling of the geometry and the field. We have reconstructed a form of f (R, T φ ) by requiring the conservation of energy-momentum tensor of the scalar field. The behavior of the reconstructed f (R, T φ ) gravity is examined for a flat potential as well as a massless scalar field model. The evolution of the universe is studied via the deceleration and equation of state parameters. The promising feature of the model is the transition behavior of the universe from deceleration to the present acceleration.

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“…In Refs. [20][21][22], the authors described the power-law cosmic expansion in higher derivative gravity. Harko et al [23] included the trace of the Stressenergy tensor in the action along with the Ricci scalar and developed a new theory named ` theory'.…”

Section: Introductionmentioning

confidence: 99%

-gravity in the context of dark energy with power law expansion and energy conditions*

Manna¹,

Panda²,

Karmakar³

et al. 2023

Chinese Phys. C

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The motto of this work is to generate a general formalism of $f(\bar{R}, L(X))-$gravity in the context of dark energy under the framework of the {\bf K-}essence emergent geometry with the Dirac-Born-Infeld (DBI) variety of action, where $\bar{R}$ is the familiar Ricci scalar, $L(X)$ is the DBI type non-canonical Lagrangian with $X={1\over 2}g^{\mu\nu}\nabla_{\mu}\phi\nabla_{\nu}\phi$ and $\phi$ is the {\bf K-}essence scalar field. The emergent gravity metric $\G_{\mu\nu}$ and the well known gravitational metric $g_{\mu\nu}$ are not conformally equivalent. We have constructed a modified field equation using the metric formalism in $f(\bar{R}, L(X))$-gravity incorporating the corresponding Friedmann equations in the framework of the background gravitational metric which is of Friedmann-Lema{\^i}tre-Robertson-Walker (FLRW) type. The solution of modified Friedmann equations have been deduced for the specific choice of $f(\bar{R}, L(X))$, which is of Starobinsky-type, using power law expansion method. The consistency of the model with the accelerating phase of the Universe has been shown, when we restrict ourselves to consider the value of the dark energy density, as $\dot\phi^{2}=\frac{8}{9}=0.888 <1$, which indicates that the present Universe is dark energy dominated. Graphical plots for the energy density ($\rho$), pressure ($p$) and equation of state parameter ($\o$) w.r.t. time ($t$) based on parametric values are interestingly consistent with the dark energy domination and hence accelerating features. We also put some light on the corresponding energy conditions and constraints of the $f(\bar{R}, L(X))$ theory with one basic example.

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Power-Law Expansion and Scalar Field Cosmology in Higher Derivative Theory

Cited by 8 publications

References 32 publications

Plane symmetric model in f(R, T) gravity

Plane symmetric model in f(R, T) gravity

The $$f(R,T^\phi )$$ f ( R , T ϕ ) gravity models with conservation of energy–momentum tensor

-gravity in the context of dark energy with power law expansion and energy conditions*

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