Dark Energy Models in f(R, T) Theory with Variable Deceleration Parameter

Mishra, R. K.; Chand, Avtar; Pradhan, Anirudh

doi:10.1007/s10773-015-2766-0

Cited by 51 publications

(14 citation statements)

References 30 publications

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“…Alternative gravity theories generalize the Einstein-Hilbert action, allowing it to depend generically on the Ricci scalar R and other scalars. Some quite interesting dark energy models have been derived from such formulations, e.g., based on f (R) [51][52][53] and f (R, T ) gravity theories [54][55][56][57][58][59], with T being the trace of the energymomentum tensor.…”

Section: Introductionmentioning

confidence: 99%

Physical Acceptability of the Renyi, Tsallis and Sharma-Mittal Holographic Dark Energy Models in the f(T,B) Gravity under Hubble’s Cutoff

2021

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In the present article, we investigate the physical acceptability of the spatially homogeneous and isotropic Friedmann–Lemâitre–Robertson–Walker line element filled with two fluids, with the first being pressureless matter and the second being different types of holographic dark energy. This geometric and material content is considered within the gravitational field equations of the f(T,B) (where T is the torsion scalar and the B is the boundary term) gravity in Hubble’s cut-off. The cosmological parameters, such as the Equation of State (EoS) parameter, during the cosmic evolution, are calculated. The models are stable throughout the universe expansion. The region in which the model is presented is dependent on the real parameter δ of holographic dark energies. For all δ≥4.5, the models vary from ΛCDM era to the quintessence era.

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Section: Introductionmentioning

confidence: 99%

Physical Acceptability of the Renyi, Tsallis and Sharma-Mittal Holographic Dark Energy Models in the f(T,B) Gravity under Hubble’s Cutoff

2021

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“…In this context, Sahoo and Sivakumar [36] have studied f (R, T ) theory in LRS Bianchi type-I universe and they have presented the big rip singularity in this theory. Mishra et al [37] have investigated homogeneous and anisotropic Bianchi type-II universe for dark energy with/without a magnetic field in f (R, T ) gravitation theory. C ¸aglar and Aygün [38] have obtained homogeneous and anisotropic Bianchi type-I solutions in f (R, T ) gravity with quark matter and Λ. Adhav [39] studied LRS Bianchi type-I universe model in f (R, T ) theory.…”

Section: Introductionmentioning

confidence: 99%

Magnetized strange quark matter in f ( R, T ) gravity with bilinear and special form of time varying deceleration parameter

2018

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In this paper, we have studied homogeneous and anisotropic locally rotationally symmetric (LRS) Bianchi type-I model with magnetized strange quark matter (MSQM) distribution and cosmological constant Λ in f (R, T ) gravity where R is the Ricci scalar and T the trace of matter source. The exact solutions of the field equations are obtained under bilinear and special form of time varying deceleration parameter (DP). Firstly, we have considered two specific forms of bilinear DP with a single parameter of the form: q = α(1−t) 1+t and q = − αt 1+t , which leads to the constant or linear nature of the function based on the constant α. Second one is the special form of the DP as q = −1 + β 1+a β . From the results obtained here, one can observe that in the early universe magnetic flux has more effects and it reduces gradually in the later stage. For t → ∞, we get p → −Bc and ρ → Bc. The behaviour of strange quark matter along with magnetic epoch gives an idea of accelerated expansion of the universe as per the observations of the type Ia Supernovae.The theoretical arguments for the late-time cosmic acceleration are being a major issue among cosmologist of the twentieth century. The idea of this accelerated expansion of universe was discovered nearly 20 years ago by observations through Supernovae Ia [1-5], CMB [6,7], baryon acoustic oscillation (BAO) in galaxy clustering [8][9][10] and WMAP [11] etc. To investigate the nature of the universe, modern cosmology continues to test the above predictions, which leads to the refinement of cosmological models. The nature and behaviour of some unknown mechanism of the universe are responsible for this accelerated expansion, commonly referred as dark energy and contains more energy budget of the universe along with negative pressure. It triggers one of the important issue to study the current acceleration of the universe.Instead of resorting the mysterious concept of dark energy, there is an alternative way to reproduce the dynamics of the expanding universe through modified theories of gravity which is an extension of general relativity. These modifications can occur in several ways such as: one can use a base as the torsional formulation of general relativity called the teleparallel gravity equivalent to general relativity [12] e.g. f (T ) gravity, where T is the torsion scalar. On the other hand one can start the curvature formulation of general relativity in Einstein-Hilbert action by replacing the Ricci scalar with its arbitrary functions or even more complicated curvature invariants such as: f (R), f (R, G) gravity, and the latest f (R, T ) gravity proposed by Harko et al. [13]. The matter Lagrangian of f (R, T ) gravity coupled with Ricci scalar R and trace of energy-momentum tensor T . Such Lagrangian with matter content will differ from the Einstein's one. It has much significance to study late-time cosmic acceleration as well as dark energy and dark matter problem [14][15][16][17]. Hypothetically matter plays more fundamental role in the description of gravitational eff...

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“…This interesting feature is a consequence of the remarkable hyperbolic solution obtained for the scale factor. While we have obtained such a feature from the model, some other approaches use this solution as a prior ansatz [107,108,109,110,111,112]. This kind of hyperbolic solution also is found in the flat ΛCDM concordance model, by neglecting radiation.…”

Section: Discussionmentioning

confidence: 65%

A unique equation of state for the universe evolution from AdS$_5$ space-time

Moraes¹,

Paula²,

Jesus³

et al. 2019

Preprint

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We apply the Induced Matter Model to a five-dimensional metric. For the case with null cosmological constant, we obtain a solution able to describe the radiation-dominated era of the universe. The positive Λ case yields a bounce cosmological model. In the negative five-dimensional cosmological constant case, the scale factor is obtained as a(t) ∼ √ sinh t, which is able to describe not only the late-time cosmic acceleration but also the non-accelerated stages of the cosmic expansion in a continuous form. This solution together with the extra-dimensional scale factor solution yields the material content of the model to be remarkably related through an equation of state analogous to the renowned MIT bag model equation of state for quark matter p = (ρ − 4B)/3. In our case, ρ = ρ m + B, with ρ m being the energy density of relativistic and nonrelativistic matter and B = |Λ|/16π represents the bag energy constant, which plays the role of the dark energy in the four-dimensional universe, with Λ being the cosmological constant of the AdS 5 space-time. Our model satisfactorily fits the observational data for the low redshift sample of the experimental measurement of the Hubble parameter, which resulted in H 0 = 72.2 +5.3 −5.5 km s −1 Mpc −1 .

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Dark Energy Models in f(R, T) Theory with Variable Deceleration Parameter

Cited by 51 publications

References 30 publications

Physical Acceptability of the Renyi, Tsallis and Sharma-Mittal Holographic Dark Energy Models in the f(T,B) Gravity under Hubble’s Cutoff

Physical Acceptability of the Renyi, Tsallis and Sharma-Mittal Holographic Dark Energy Models in the f(T,B) Gravity under Hubble’s Cutoff

Magnetized strange quark matter in f ( R, T ) gravity with bilinear and special form of time varying deceleration parameter

A unique equation of state for the universe evolution from AdS$_5$ space-time

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