Locally rotationally symmetric Bianchi type I cosmology in f(R, T) gravity

Shamir, M. Farasat

doi:10.1140/epjc/s10052-015-3582-7

Cited by 159 publications

(85 citation statements)

References 90 publications

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“…Till the present time, different cosmological aspects have been addressed in f (R, T ) gravity including reconstruction schemes, anisotropic solutions, energy conditions, thermodynamics, viscous solutions, phase space perturbations and stability, etc. [15][16][17][18][19][20][21][22][23][24][25][26][27][28][29][30][31][32].…”

Section: Introductionmentioning

confidence: 99%

Static spherically symmetric wormholes in f(R, T) gravity

2016

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In this work, we explore wormhole solutions in f (R, T ) theory of gravity, where R is the scalar curvature and T is the trace of stress-energy tensor of matter. To investigate this, we consider a static spherically symmetric geometry with matter contents as anisotropic, isotropic, and barotropic fluids in three separate cases. By taking into account the Starobinsky f (R) model, we analyze the behavior of energy conditions for these different kinds of fluids. It is shown that the wormhole solutions can be constructed without exotic matter in few regions of space-time. We also give the graphical illustration of the results obtained and discuss the equilibrium picture for the anisotropic case only. It is concluded that the wormhole solutions with anisotropic matter are realistic and stable in this theory of gravity.

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Section: Introductionmentioning

confidence: 99%

Static spherically symmetric wormholes in f(R, T) gravity

2016

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“…It has been argued that such a dependence on T may come from the presence of an imperfect fluid or quantum effects. Many cosmological applications based on f (R, T ) gravity can be found in [44][45][46][47][48][49][50][51][52][53][54][55][56][57].…”

Section: Introductionmentioning

confidence: 99%

Compact stars in $$f(R,\mathcal {T})$$ f ( R , T ) gravity

et al. 2016

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In the present paper we generate a set of solutions describing the interior of a compact star under f (R, T ) theory of gravity which admits conformal motion. An extension of general relativity, the f (R, T ) gravity is associated to Ricci scalar R and the trace of the energy-momentum tensor T . To handle the Einstein field equations in the form of differential equations of second order, first of all we adopt the Lie algebra with conformal Killing vectors (CKV) which enable one to get a solvable form of such equations and second we consider the equation of state (EOS) p = ωρ with 0 < ω < 1 for the fluid distribution consisting of normal matter, ω being the EOS parameter. We therefore analytically explore several physical aspects of the model to represent behavior of the compact stars such as-energy conditions, TOV equation, stability of the system, Buchdahl condition, compactness and redshift. It is checked that the physical validity and the acceptability of the present model within the specified observational constraint in connection to a dozen of the compact star candidates are quite satisfactory.

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“…Although the late-time acceleration of the universe expansion [13][14][15] has been broadly investigated in such a theory of gravity [16][17][18][19][20][21][22][23][24][25], the inflationary era still presents a lack of examination. The same happens for the radiation-dominated era of the universe.…”

Section: Introductionmentioning

confidence: 99%

“…Such an EoS yields a null trace for the energy-momentum tensor of a perfect fluid. A null trace for the energy-momentum tensor yields the f (R) formalism for the f (R, T ) functional forms found in the literature (see, for instance, [12,[16][17][18][19][20][21][22][23][24][25]). Hence the study of the radiation era of the universe in f (R, T ) gravity seems to be quite tricky.…”

Section: Introductionmentioning

confidence: 99%

A complete cosmological scenario from $$f(R,T^{\phi })$$ f ( R , T ϕ )

Moraes¹,

Santos²

2016

Eur. Phys. J. C

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Recent elaborated by Harko et al., the f (R, T ) theories of gravity allow one to contemplate an optimistic alternative to dark energy, for which R and T stand for the Ricci scalar and the trace of the energy-momentum tensor, respectively. Although the literature has shown that the T dependence on the gravitational part of the action -which is due to the consideration of quantum effects -may induce some novel features in the scope of late-time cosmological dynamics, in the radiation-dominated universe, when T = 0, no contributions seem to arise from such theories. Apparently, f (R, T ) contributions to a radiation-dominated universe may arise only from the f (R, T φ ) approach, which is nothing but the f (R, T ) gravity in the case of a selfinteracting scalar field whose trace of the energy-momentum tensor is T φ . We intend, in this article, to show how f (R, T φ ) theories of gravity can contribute to the study of the primordial stages of the universe. Our results predict a graceful exit from an inflationary stage to a radiation-dominated era. They also predict a late-time cosmic acceleration after a matter-dominated phase, enabling the f (R, T φ ) theories to describe, in a self-consistent way, all the different stages of the dynamics of the universe.

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Locally rotationally symmetric Bianchi type I cosmology in f(R, T) gravity

Cited by 159 publications

References 90 publications

Static spherically symmetric wormholes in f(R, T) gravity

Static spherically symmetric wormholes in f(R, T) gravity

Compact stars in $$f(R,\mathcal {T})$$ f ( R , T ) gravity

A complete cosmological scenario from $$f(R,T^{\phi })$$ f ( R , T ϕ )

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