Holographic dark energy reconstruction in f ( T , T ) $f(T,\mathcal{T})$ gravity

Salako, Ines G.; Jawad, Abdul; Chattopadhyay, Surajit

doi:10.1007/s10509-015-2406-4

Cited by 44 publications

(17 citation statements)

References 67 publications

(82 reference statements)

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“…Let us now study the cosmological applications of f (T, T ) gravity, both at early and late times, following [617] (see also [624,[628][629][630][631]). In particular, we proceed to the investigation of some specific f (T, T ) ansatzen, focusing on the evolution of observables such as the various density parameters Ω i = 8πGρ i /(3H 2 ) and the dark energy equation-of-state parameter w DE .…”

Section: Cosmological Behaviormentioning

confidence: 99%

f(T) teleparallel gravity and cosmology

et al. 2016

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Over the past decades, the role of torsion in gravity has been extensively investigated along the main direction of bringing gravity closer to its gauge formulation and incorporating spin in a geometric description. Here we review various torsional constructions, from teleparallel, to Einstein-Cartan, and metric-affine gauge theories, resulting in extending torsional gravity in the paradigm of f (T ) gravity, where f (T ) is an arbitrary function of the torsion scalar. Based on this theory, we further review the corresponding cosmological and astrophysical applications. In particular, we study cosmological solutions arising from f (T ) gravity, both at the background and perturbation levels, in different eras along the cosmic expansion. The f (T ) gravity construction can provide a theoretical interpretation of the late-time universe acceleration, alternative to a cosmological constant, and it can easily accommodate with the regular thermal expanding history including the radiation and cold dark matter dominated phases. Furthermore, if one traces back to very early times, for a certain class of f (T ) models, a sufficiently long period of inflation can be achieved and hence can be investigated by cosmic microwave background observations, or alternatively, the Big Bang singularity can be avoided at even earlier moments due to the appearance of non-singular bounces. Various observational constraints, especially the bounds coming from the large-scale structure data in the case of f (T ) cosmology, as well as the behavior of gravitational waves, are described in detail. Moreover, the spherically symmetric and black hole solutions of the theory are reviewed. Additionally, we discuss various extensions of the f (T ) paradigm. Finally, we consider the relation with other modified gravitational theories, such as those based on curvature, like f (R) gravity, trying to enlighten the subject of which formulation, or combination of formulations, might be more suitable for quantization ventures and cosmological applications. Contents

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Section: Cosmological Behaviormentioning

confidence: 99%

f(T) teleparallel gravity and cosmology

et al. 2016

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“…The modification has been done by changing the geometrical part of the Einstein field equations (EFE), i.e., the action is modified by considering a generalized functional form of gravitational Lagrangian density. Some of the well known relevant alternative theories of gravitation are f (R) gravity [21][22][23][24][25], f (T) gravity [26,27], f (R, T ) gravity [28][29][30][31][32][33][34][35][36], f (T, T ) gravity [37][38][39][40][41][42], f (G) gravity [43][44][45] and f (R, G) gravity [46] where R, T, T and G are scalar curvature, torsion scalar, trace of the energy momentum tensor and Gauss-Bonnet scalar respectively.…”

Section: Introductionmentioning

confidence: 99%

Anisotropic strange star with Tolman–Kuchowicz metric under f(R, T) gravity

et al. 2020

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In the current article, we study anisotropic spherically symmetric strange star under the background of f (R, T ) gravity using the metric potentials of Tolman-Kuchowicz type [1,2] as λ(r) = ln(1 + ar 2 + br 4 ) and ν(r) = Br 2 + 2 ln C which are free from singularity, satisfy stability criteria and also well behaved. We calculate the value of constants a, b, B and C using matching conditions and the observed values of the masses and radii of known samples. To describe the strange quark matter (SQM) distribution, here we have used the phenomenological MIT bag model equation of state (EOS) where the density profile (ρ) is related to the radial pressure (p r ) as p r (r) = 1 3 (ρ − 4B g ). Here quark pressure is responsible for generation of bag constant B g . Motivation behind this study lies in finding out a nonsingular physically acceptable solution having various properties of strange stars. The model shows consistency with various energy conditions, TOV equation, Herrera's cracking condition and also with Harrison-Zel ′ dovich-Novikov's static stability criteria. Numerical values of EOS parameter and the adiabatic index also enhance the acceptability of our model.

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“…Holographic reconstruction of modified gravity has already been reported in the cosmological literature. Various authors [40,41,[46][47][48] have reconstructed different candidates of modified gravity from holographic dark energy (HDE) with different IR cut-offs.…”

Section: Introductionmentioning

confidence: 99%

Reconstructed f(R) Gravity and Its Cosmological Consequences in theChameleon Scalar Field with a Scale Factor Describing the Pre-Bounce Ekpyrotic Contraction

et al. 2020

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The present study reports a reconstruction scheme for f(R) gravity with the scale factor a(t)∝(t*−t)2c2 describing the pre-bounce ekpyrotic contraction, where t* is the big crunch time. The reconstructed f(R) is used to derive expressions for density and pressure contributions, and the equation of state parameter resulting from this reconstruction is found to behave like “quintom”. It has also been observed that the reconstructed f(R) has satisfied a sufficient condition for a realistic model. In the subsequent phase, the reconstructed f(R) is applied to the model of the chameleon scalar field, and the scalar field ϕ and the potential V(ϕ) are tested for quasi-exponential expansion. It has been observed that although the reconstructed f(R) satisfies one of the sufficient conditions for realistic model, the quasi-exponential expansion is not available due to this reconstruction. Finally, the consequences of pre-bounce ekpyrotic inflation in f(R) gravity are compared to the background solution for f(R) matter bounce.

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Holographic dark energy reconstruction in f ( T , T ) $f(T,\mathcal{T})$ gravity

Cited by 44 publications

References 67 publications

f(T) teleparallel gravity and cosmology

f(T) teleparallel gravity and cosmology

Anisotropic strange star with Tolman–Kuchowicz metric under f(R, T) gravity

Reconstructed f(R) Gravity and Its Cosmological Consequences in theChameleon Scalar Field with a Scale Factor Describing the Pre-Bounce Ekpyrotic Contraction

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