Energy conditions in generalized teleparallel gravity models

Jamil, Mubasher; Momeni, Davood; Myrzakulov, Ratbay

doi:10.1007/s10714-012-1472-y

Cited by 60 publications

(19 citation statements)

References 69 publications

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“…The theory seems interesting as it may explain the current cosmic acceleration without involving the dark energy. Some researchers have done a considerable amount of work in this theory so far [16][17][18][19][20][21][22][23][24][25]. Another extended theory, known as f (R) theory of gravity, has also attracted attention of the researchers in recent years.…”

Section: Introductionmentioning

confidence: 99%

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

Shamir

2015

Eur. Phys. J. C

172

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This manuscript is devoted to the investigation of the Bianchi type I universe in the context of f (R, T ) gravity. For this purpose, we explore the exact solutions of locally rotationally symmetric Bianchi type I spacetime. The modified field equations are solved by assuming an expansion scalar θ proportional to the shear scalar σ , which gives A = B n , where A, B are the metric coefficients and n is an arbitrary constant. In particular, three solutions have been found and physical quantities are calculated in each case.

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Section: Introductionmentioning

confidence: 99%

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

Shamir

2015

Eur. Phys. J. C

172

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“…(76), we have used Eq. (42). Now, we will check the consistency of the found results with those of the GR by choosing the special case f (T, T ) = −2Λ.…”

Section: Null Vector Fields With Flrw Backgroundmentioning

confidence: 85%

Geodesic Deviation Equation in ΛCDM f ( T , T ) $f(T,\mathcal {T})$ Gravity

et al. 2016

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The geodesic deviation equation has been investigated in the framework of f (T, T ) gravity, where T denotes the torsion and T is the trace of the energy-momentum tensor, respectively. The FRW metric is assumed and the geodesic deviation equation has been established following the General Relativity approach in the first hand and secondly, by a direct method using the modified Friedmann equations. Via fundamental observers and null vector fields with FRW background, we have generalized the Raychaudhuri equation and the Mattig relation in f (T, T ) gravity. Furthermore, we have numerically solved the geodesic deviation equation for null vector fields by considering a particular form of f (T, T ) which induces interesting results susceptible to be tested with observational data.

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“…For specific coupling functions and potentials its flat Friedmann-Lemaître-Robertson-Walker (FLRW) cosmology has been scrutinized by phase space analysis [17][18][19][20], while some analytic solutions were found under particular Ansätze [21,22] or by employing the Noether symmetry method [23]. Other studies discuss parameter fit with cosmological observations [24], growth of density perturbations [25], energy conditions [26], and the possibility of singularities [27].…”

Section: Introductionmentioning

confidence: 99%

General relativity as an attractor for scalar-torsion cosmology

Järv

Toporensky

2016

Phys. Rev. D

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We study flat Friedmann-Lemaître-Robertson-Walker cosmological models for a scalar field coupled nonminimally to teleparallel gravity with generic coupling and potential functions. The goal of this paper is to determine the conditions under which cosmological evolution tends to the limit where the variation of the gravitational "constant" ceases and the system evolves close to general relativity. These conditions can be read off from the approximate analytical solutions describing the process in matter and potential domination eras. Only those models where the GR limit exists and is an attractor can be considered viable. We expect the results to hold in the original "pure tetrad" formulation as well as in the recently suggested covariant formulation of the teleparallel theory. In the former case the GR attractor simultaneously provides a mechanism how cosmological evolution suppresses the problematic degrees of freedom stemming from the lack of local Lorentz invariance.PACS numbers: 04.50. Kd, 95.36.+x

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Energy conditions in generalized teleparallel gravity models

Cited by 60 publications

References 69 publications

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

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

Geodesic Deviation Equation in ΛCDM f ( T , T ) $f(T,\mathcal {T})$ Gravity

General relativity as an attractor for scalar-torsion cosmology

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