Evolution of axially symmetric anisotropic sources in f(R, T) gravity

Zubair, M.; Noureen, Ifra

doi:10.1140/epjc/s10052-015-3496-4

Cited by 108 publications

(59 citation statements)

References 39 publications

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“…[58][59][60][61][62][63][64][65]. Sharif et al [58] have discussed the stability of a collapsing spherical body of an isotropic fluid distribution considering the non-static spherically symmetric line element.…”

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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Section: Introductionmentioning

confidence: 99%

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

et al. 2016

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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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“…The field equations of f (R, T ) modified theory have been explored by implementing the perturbation approach [46]. The possible formation of compacts stars in a modified theory of gravity by using the Krori and Barua metric for spherically symmetric anisotropic compact stars has been discussed [47,48]. In a recently published paper [1], Sharif and Ikram presented a new modified f (G, T ) theory of gravity and studied various energy conditions for the FriedmannRobertson-Walker (FRW) universe.…”

Section: Introductionmentioning

confidence: 99%

Emerging anisotropic compact stars in $$f(\mathcal {G},T)$$ f ( G , T ) gravity

Shamir

Ahmad

2017

Eur. Phys. J. C

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The possible emergence of compact stars has been investigated in the recently introduced modified GaussBonnet f (G, T ) gravity, where G is the Gauss-Bonnet term and T is the trace of the energy-momentum tensor (Sharif and Ikram, Eur Phys J C 76:640, 2016). Specifically, for this modified f (G, T ) theory, the analytic solutions of Krori and Barua have been applied to an anisotropic matter distribution. To determine the unknown constants appearing in the Krori and Barua metric, the well-known three models of the compact stars, namely 4U1820-30, Her X-I, and SAX J 1808.4-3658 have been used. The analysis of the physical behaviour of the compact stars has been presented and the physical features like energy density and pressure, energy conditions, static equilibrium, stability, measure of anisotropy, and regularity of the compact stars, have been discussed.

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Evolution of axially symmetric anisotropic sources in f(R, T) gravity

Cited by 108 publications

References 39 publications

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

Emerging anisotropic compact stars in $$f(\mathcal {G},T)$$ f ( G , T ) gravity

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