The trace of the trace of the energy–momentum tensor-dependent Einstein’s field equations

Moraes, P. H. R. S.

doi:10.1140/epjc/s10052-019-7195-4

Cited by 17 publications

(3 citation statements)

References 149 publications

(167 reference statements)

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“…Harko et al have demonstrated that the covariant derivative of energy-momentum tensor does not vanish in the theory giving the non-geodesic motion of a massive test particle and also it has been noted that an extra force remains effective because of the matter-geometry coupling developed in the theory. Later, Moraes presented that the extra force may vanish for L m = − p in the non-relativistic dust matter case [42]. Under analogous noninteracting two fluid structures as presented by Harko et al, S. Chakraborty has described [43] that the conservation of energy-momentum tensor can be taken into account for some specific forms of the f (R, T ) function.…”

Section: Introductionmentioning

confidence: 95%

“…It is to be noted that because of the extra terms appearing in the field equations, the f (R, T ) theory of gravity can be regarded as a two fluid model [42]. Further, defining T I µν for an anisotropic geometric matter distribution, we can express it as [29] T νI µ = diag −ρ I , P I r , P I t , P I t ,…”

Section: Modified Einstein Field Equations In F (R T ) Gravitymentioning

confidence: 99%

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Galactic rotation curves of spiral galaxies and dark matter in $f(\mathcal{R},T)$ gravity theory

Mohan¹,

Goswami²

2022

Preprint

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Galactic rotation curve is a powerful indicator of the state of the gravitational field within a galaxy. Flatness of these curves implies the linear increase of mass to have constant velocity with the radial distance. In this paper, we focus on the possibility of explaining the flatness of observed rotation curves of spiral galaxies without postulating the existence of dark matter in the framework of f (R, T ) gravity where the gravitational Lagrangian is written by an arbitrary function of R, the Ricci scalar and of T , the trace of stress-energy tensor Tµν . We derive the gravitational field equations in this gravity theory for the static spherically symmetric spacetime and solve the equations for metric coefficients using a specific model that has minimal coupling between matter and geometry. The orbital motion of a massive test particle moving in a stable circular orbit is considered and the behaviour of tangential velocity in the halo region with the help of the considered model is studied. The linear variation with distance of the interaction mass generated due to matter-geometry coupling successfully explains the galactic dynamics without the existence of dark matter at large distances from the galactic core.

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Section: Introductionmentioning

confidence: 95%

Section: Modified Einstein Field Equations In F (R T ) Gravitymentioning

confidence: 99%

Galactic rotation curves of spiral galaxies and dark matter in $f(\mathcal{R},T)$ gravity theory

Mohan¹,

Goswami²

2022

Preprint

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“…Since the choice of the matter Lagrangian L m = −p sq is not unique for a perfect fluid, Moraes [63] has eliminated this arbitrariness by deriving the following matter Lagrangian:…”

Section: The Model and Field Equationsmentioning

confidence: 99%

Plane Symmetric Cosmological Model with Strange Quark Matter in f(R,T) Gravity

Singh,

Jokweni,

Beesham

2023

Universe

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A plane symmetric Bianchi-I model filled with strange quark matter (SQM) was explored in f(R,T)=R+2λT gravity, where R is the Ricci scalar, T is the trace of the energy-momentum tensor, and λ is an arbitrary constant. Three different types of solutions were obtained. In each model, comparisons of the outcomes in f(R,T) gravity and bag constant were made to comprehend their roles. The first power-law solution was obtained by assuming that the expansion scalar is proportional to the shear scalar. This solution was compared with a similar one obtained earlier. The second solution was derived by assuming a constant deceleration parameter q. This led to two solutions: one power-law and the other exponential. Just as in the case of general relativity, we can obtain solutions for each of the different eras of the universe, but we cannot obtain a model which shows transitional behavior from deceleration to acceleration. However, the third solution is a hybrid solution, which shows the required transition. The models start off with anisotropy, but are shear free at late times. In general relativity, the effect of SQM is to accelerate the universe, so we expect the same in f(R,T) gravity.

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Einstein’s vacuum field equation: lumps, manifold periodic, generalized breathers, interactions and rogue wave solutions

et al. 2023

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The trace of the trace of the energy–momentum tensor-dependent Einstein’s field equations

Cited by 17 publications

References 149 publications

Galactic rotation curves of spiral galaxies and dark matter in $f(\mathcal{R},T)$ gravity theory

Galactic rotation curves of spiral galaxies and dark matter in $f(\mathcal{R},T)$ gravity theory

Plane Symmetric Cosmological Model with Strange Quark Matter in f(R,T) Gravity

Einstein’s vacuum field equation: lumps, manifold periodic, generalized breathers, interactions and rogue wave solutions

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