Accelerating universe from F(T) gravity

Myrzakulov, Ratbay

doi:10.1140/epjc/s10052-011-1752-9

Cited by 368 publications

(224 citation statements)

References 65 publications

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“…At first, f (T )-gravity was proposed as models for inflation [28,29]. Then, models based on f (T )-gravity was considered to describe the present accelerating expansion of the universe without resorting to dark energy (DE) [30][31][32][33][34][35][36][37][38][39][40][41][42][43]. Also, thermodynamics of f (T )-gravity models has been investigated in [44][45][46].…”

Section: Jhep01(2016)131mentioning

confidence: 99%

Power-law and intermediate inflationary models in f(T)-gravity

Rezazadeh

Abdolmaleki

Karami

2016

J. High Energ. Phys.

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We study inflation in the framework of f (T )-gravity in the presence of a canonical scalar field. After reviewing the basic equations governing the background cosmology in f (T )-gravity, we turn to study the cosmological perturbations and obtain the evolutionary equations for the scalar and tensor perturbations. Solving those equations, we find the power spectra for the scalar and tensor perturbations. Then, we consider a power-law f (T ) function and investigate the inflationary models with the power-law and intermediate scale factors. We see that in contrast with the standard inflationary scenario based on the Einstein gravity, the power-law and intermediate inflationary models in f (T )-gravity can be compatible with the observational results of Planck 2015 at 68% CL. We find that in our f (T ) setting, the potentials responsible for the both power-law and intermediate inflationary models have the power-law form V (φ) ∝ φ m but the power m is different for them. Therefore, we can refine some of power-law inflationary potentials in the framework of f (T )-gravity while they are disfavored by the observational data in the standard inflationary scenario. Interestingly enough, is that the self-interacting quartic potential V (φ) ∝ φ 4 which has special reheating properties, can be consistent with the Planck 2015 data in our f (T ) scenario while it is ruled out in the standard inflationary scenario.

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Section: Jhep01(2016)131mentioning

confidence: 99%

Power-law and intermediate inflationary models in f(T)-gravity

Rezazadeh

Abdolmaleki

Karami

2016

J. High Energ. Phys.

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“…Note that choosing β = 0 (or (T ) = 0) leads to teleparallel gravity which is equivalent to General Relativity. Note that this choice (T ) = β √ −T has correspondence with the cosmological constant EoS in (T ) gravity [77]. This (T ) model can be recovered via reconstruction scheme of holographic dark energy [84].…”

Section: Stability Analysis Of Perfect Fluidmentioning

confidence: 91%

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

Jamil¹,

Yesmakhanova

Momeni

et al. 2012

Open Physics

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Abstract:In this paper, we examine the interacting dark energy model in (T ) cosmology. We assume dark energy as a perfect fluid and choose a specific cosmologically viable form (T ) = β √ T . We show that there is one attractor solution to the dynamical equation of (T ) Friedmann equations. Further we investigate the stability in phase space for a general (T ) model with two interacting fluids. By studying the local stability near the critical points, we show that the critical points lie on the sheet * = ( − 1) * in the phase space, spanned by coordinates ( Ω T ). From this critical sheet, we conclude that the coupling between the dark energy and matter ∈ (−2 0). PACS (2008):

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“…(ii) The case of (k = 0, f (T ) = T ), it reduces to [64]. (iii) The case of (k = 0, f (T ) = T ), this case shows the dynamical evolution in non-flat models [33].…”

Section: F (T ) Cosmologymentioning

confidence: 99%

Reconstruction of f ( T ) $f(T)$ -gravity in the absence of matter

Hanafy¹,

Nashed²

2016

Astrophys Space Sci

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We derive an exact f (T ) gravity in the absence of ordinary matter in Friedmann-RobertsonWalker (FRW) universe, where T is the teleparallel torsion scalar. We show that vanishing of the energy-momentum tensor T µν of matter does not imply vanishing of the teleparallel torsion scalar, in contrast to general relativity, where the Ricci scalar vanishes. The theory provides an exponential (inflationary) scale factor independent of the choice of the sectional curvature. In addition, the obtained f (T ) acts just like cosmological constant in the flat space model. Nevertheless, it is dynamical in non-flat models. In particular, the open universe provides a decaying pattern of the f (T ) contributing directly to solve the fine-tuning problem of the cosmological constant. The equation of state (EoS) of the torsion vacuum fluid has been studied in positive and negative Hubble regimes. We study the case when the torsion is made of a scalar field (tlaplon) which acts as torsion potential. This treatment enables to induce a tlaplon field sensitive to the symmetry of the spacetime in addition to the reconstruction of its effective potential from the f (T ) theory. The theory provides six different versions of inflationary models. The real solutions are mainly quadratic, the complex solutions, remarkably, provide Higgs-like potential.PACS numbers: 98.80.Qc, 04.20.Cv, 98.80.Cq.

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Accelerating universe from F(T) gravity

Cited by 368 publications

References 65 publications

Power-law and intermediate inflationary models in f(T)-gravity

Power-law and intermediate inflationary models in f(T)-gravity

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

Reconstruction of f ( T ) $f(T)$ -gravity in the absence of matter

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