Phase space analysis of interacting dark energy in f(T) cosmology

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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“…Correspondingly, inserting the above vierbein into the torsion tensor (228) and into the contorsion tensor (232) we obtain their components as…”

Section: E Anisotropic Cosmologymentioning

confidence: 99%

f(T) teleparallel gravity and cosmology

et al. 2016

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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

167

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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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“…P 44 is stable forω < −1 and b > 1 9 . It is also possible to determine the stability of point P 45 . The stabilities of the point P 47 and also P 35 from the model III are not easy to be studied because the matrix of Jacobi in these cases is not diagonal and the behaviors of its eigenvalues are not trivial.…”

Section: Interacting Model -Ivmentioning

confidence: 99%

f ( T , T ) $f(T,\mathcal{T})$ cosmological models in phase space

Ganiou

Salako

Houndjo

et al. 2016

Astrophys Space Sci

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In this paper we explore f (T, T ), where T and T denote the torsion scalar and the trace of the energy-momentum tensor respectively. We impose the covariant conservation to the energymomentum tensor and obtain a cosmological f (T, T ) respectively. We impose the covariant conservation to the energy-momentum tensor and obtain a cosmological f (T, T ) model. Then, we study the stability of the obtained model for power-law and de Sitter solutions and our result show that the model can be stable for some values of the input parameters, for both power-law and de Sitter solutions.

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Phase space analysis of interacting dark energy in f(T) cosmology

Cited by 73 publications

References 84 publications

f(T) teleparallel gravity and cosmology

f(T) teleparallel gravity and cosmology

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

f ( T , T ) $f(T,\mathcal{T})$ cosmological models in phase space

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