Bianchi type I cosmology in generalized Saez–Ballester theory via Noether gauge symmetry

Jamil, Mubasher; Ali, Sajid; Momeni, Davood; Myrzakulov, Ratbay

doi:10.1140/epjc/s10052-012-1998-x

Cited by 71 publications

(18 citation statements)

References 49 publications

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“…The WiggleZ-data [63] indicates the following information about A and z b : A = 0.474±0.034, 0.442 ± 0.020 and 0.424 ± 0.021 for the redshifts z b = 0.44, 0.60 and 0.73, respectively. The key quantity of a statistical analysis is the χ 2 parameter,…”

Section: Observational Constraints On Interacting Models With Varying λmentioning

confidence: 99%

Interacting Quintessence Dark Energy Models in Lyra Manifold

Khurshudyan

Sadeghi

Myrzakulov

et al. 2014

Advances in High Energy Physics

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In this paper, we consider two-component dark energy models in Lyra manifold. The first component is assumed as a quintessence field while the second component may be a viscous polytropic gas, a viscous Van der Waals gas or a viscous modified Chaplygin gas. We also consider the possibility of interaction between components. By using the numerical analysis, we study some cosmological parameters of the models and compare them with observational data.

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Section: Observational Constraints On Interacting Models With Varying λmentioning

confidence: 99%

Interacting Quintessence Dark Energy Models in Lyra Manifold

Khurshudyan

Sadeghi

Myrzakulov

et al. 2014

Advances in High Energy Physics

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“…(z ϩ 1) 3 (50) and the explicit expression of H depending on cosmic time t may be obtained. By substituting (z + 1) by 1/a(t), one gets…”

Section: Time Evolutionmentioning

confidence: 99%

Realistic f(T) model describing the de Sitter epoch of the dark energy dominated universe

et al. 2015

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We consider an exponential model within the so-called f(T) theory of gravity, where T denotes the torsion scalar. We focus our attention on a cosmological feature of a f(T) model, checking whether it may describe the de Sitter stage of the current universe according to the evolution of the redshift, z. Our results show that the model reproduces the de Sitter stage only for low redshifts, where the perturbation function approached zero, whereas the effective parameter of the equation of state goes to -1, which is the expected behavior for any model able to reproduce the de Sitter stage. PACS Nos.: 98.80.-k, 04.50.Kd, 95.36.+x.Résumé : Nous nous penchons sur un modèle exponentiel à l'intérieur de la théorie f(T) de la gravité, où T est la torsion scalaire. Nous focalisons notre effort sur une caractéristique cosmologique du modèle f(T), vérifiant s'il peut décrire la période de de Sitter de notre univers actuel selon l'évolution du déplacement vers le rouge, z. Nos résultats montrent que le modèle reproduit la période de de Sitter seulement pour de faibles déplacements vers le rouge, là où la perturbation tend vers zéro, alors que le paramètre effectif de l'équation d'état tend vers -1, le comportement attendu de tout modèle capable de reproduire la période de de Sitter. [Traduit par la Rédaction]

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“…To the best of our knowledge, it has not been investigated for which values of W the observational limits can be satisfied. The SB theory and its extended versions, in both the classical and quantum levels, have been widely applied to investigate various cosmological problems in either four or arbitrary dimensions [7][8][9][10][11][12][13][14][15][16][17][18].…”

Section: Introductionmentioning

confidence: 99%

Noncommutativity, Sáez–Ballester Theory and Kinetic Inflation

Rasouli

2022

Universe

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This paper presents a noncommutative (NC) version of an extended Sáez–Ballester (SB) theory. Concretely, considering the spatially flat Friedmann–Lemaître–Robertson–Walker (FLRW) metric, we propose an appropriate dynamical deformation between the conjugate momenta and, applying the Hamiltonian formalism, obtain deformed equations of motion. In our model, the NC parameter appears linearly in the deformed Poisson bracket and the equations of the NC SB cosmology. When it goes to zero, we get the corresponding commutative counterparts. Even by restricting our attention to a particular case, where there is neither an ordinary matter nor a scalar potential, we show that the effects of the noncommutativity provide interesting results: applying numerical endeavors for very small values of the NC parameter, we show that (i) at the early times of the universe, there is an inflationary phase with a graceful exit, for which the relevant nominal condition is satisfied; (ii) for the late times, there is a zero acceleration epoch. By establishing an appropriate dynamical framework, we show that the results (i) and (ii) can be obtained for many sets of the initial conditions and the parameters of the model. Finally, we indicate that, at the level of the field equations, one may find a close resemblance between our NC model and the Starobinsky inflationary model.

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Bianchi type I cosmology in generalized Saez–Ballester theory via Noether gauge symmetry

Cited by 71 publications

References 49 publications

Interacting Quintessence Dark Energy Models in Lyra Manifold

Interacting Quintessence Dark Energy Models in Lyra Manifold

Realistic f(T) model describing the de Sitter epoch of the dark energy dominated universe

Noncommutativity, Sáez–Ballester Theory and Kinetic Inflation

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