Bouncing scenario in f(R,T) gravity

Sahoo, P. K.; Bhattacharjee, Snehasish; Tripathy, S. K.

doi:10.1142/s0217732320500959

Cited by 57 publications

(31 citation statements)

References 49 publications

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“…The purpose of the present article is to investigate inflationary cosmological solutions consistent with latest Planck and BICEP2/Keck Array data in the framework of mimetic f (R, T ) gravity with Lagrange multiplier and mimetic potential. f (R, T ) gravity was introduced in [30] and has been extremely successful in the understanding of the flat rotation curves [31], late-time acceleration [30], baryogenesis [32], bouncing cosmology [33,34], evolution of density perturbations [35], redshift drift [36], Big bang nucleosynthesis [37], temporally varying physical constants [38], inflation [20,21], and viscous cosmology [39]. The manuscript is organized as follows: In Section II, we provide an overview of mimetic f (R, T ) gravity.…”

Section: Introductionmentioning

confidence: 99%

Inflation in f(R, T) gravity

et al. 2020

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In this paper, we employ mimetic f (R, T ) gravity coupled with Lagrange multiplier and mimetic potential to yield viable inflationary cosmological solutions consistent with latest Planck and BI-CEP2/Keck Array data. We present here three viable inflationary solutions of the Hubble parameter (H) represented by H(Nwhere A, β, B, α, γ are free parameters, and N represents the number of e-foldings. We carry out the analysis with the simplest minimal f (R, T ) function of the form f (R, T ) = R + χT , where χ is the model parameter. We report that for the chosen f (R, T ) gravity model, viable cosmologies are obtained compatible with observations by conveniently setting the Lagrange multiplier and the mimetic potential.

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Section: Introductionmentioning

confidence: 99%

Inflation in f(R, T) gravity

et al. 2020

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“…Recently, P.K. Sahoo and S. Bhattacharjee (Sahoo & Bhattacharjee, 2020) investigated gravitational Baryogenesis in non-minimal coupled ( , ) gravity. Furthermore, most of the above studies are done by the prior assumptions of scale factor or followed by the parametrization techniques.…”

Section: Introductionmentioning

confidence: 99%

“…The literature includes several works with certain linear forms of ( , ) gravity (Harko & et al, 2011;Sahoo, Bhattacharjee, Tripathy, & Sahoo, 2020;Sahoo, Sahu, & Nath, 2016). We have considered the linear form of ( , ) gravity in the last second section, which demonstrates some consistency with ΛCDM and non-linear form.…”

Section: Introductionmentioning

confidence: 99%

Energy Conditions in Non-minimally Coupled $f(R,T)$ Gravity

Sahoo,

Mandal,

Arora

2022

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In today's scenario, going beyond Einstein's theory of gravity leads us to some more complete and modified gravity theories. One of them is the ( , ) gravity in which is the Ricci scalar, and is the trace of the energy-momentum tensor. Using a well-motivated linear ( , ) gravity model with a single parameter, we studied the strong energy condition (SEC), the weak energy condition (WEC), the null energy condition (NEC), and the dominant energy condition (DEC) under the simplest non-minimal matter geometry coupling with a perfect fluid distribution. The model parameter is constrained by energy conditions and a single parameter proposed equation of state (EoS), resulting in the compatibility of the ( , ) models with the accelerated expansion of the universe. It is seen that the EoS parameter illustrate the quintessence phase in a dominated accelerated phase, pinpoint to the cosmological constant yields as a prediction the phantom era. Also, the present values of the cosmological constant and the acceleration of the universe are used to check the viability of our linear ( , ) model of gravity. It is observed that the positive behavior of DEC and WEC indicates the validation of the model. In contrast, SEC is violating the condition resulting in the accelerated expansion of the universe.

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“…In this work we shall work with f (R, T) gravity theory in which the Ricci scalar R is replaced with a suitable functional form of R and trace of energy momentum tensor T [43] and therefore is a straightforward conjecture to f (R) gravity (see [44,45]). f (R, T) gravity have proved to be successful in numerous cosmological sectors such as dark matter [46] dark energy [47], massive pulsars [48,49], super-Chandrasekhar white dwarfs [50], wormholes [51][52][53][54][55][56][57][58][59][60][61], gravitational waves [62][63][64], bouncing cosmology [65,66], baryogenesis [67,68], Big-Bang nucleosynthesis [69] and in varying speed of light scenarios [70]. The article is methodized as follows: In Section II we provide a summary of f (R, T) gravity and solve the field equations assuming a bulk viscous fluid.…”

Section: Introductionmentioning

confidence: 99%

Late-time viscous cosmology in f(R, T) gravity

2021

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The article communicates an alternative route to suffice the late-time acceleration considering a bulk viscous fluid with viscosity coefficient ζ = ζ 0 + ζ 1 H + ζ 2 H 2 , where ζ 0 , ζ 1 , ζ 2 are constants in the framework of f (R, T) modified gravity. We presume the f (R, T) functional form to be f = R + 2αT where α is a constant. We then solve the field equations for the Hubble Parameter and study the cosmological dynamics of kinematic variables such as deceleration, jerk, snap and lerk parameters as a function of cosmic time. We observe the deceleration parameter to be highly sensitive to α and undergoes a signature flipping at around t ∼ 10 Gyrs for α = −0.179 which is favored by observations. The EoS parameter for our model assumes values close to −1 at t 0 = 13.7Gyrs which is in remarkable agreement with the latest Planck measurements. Next, we study the evolution of energy conditions and find that our model violate the Strong Energy Condition in order to explain the late-time cosmic acceleration. To understand the nature of dark energy mimicked by the bulk viscous baryonic fluid, we perform some geometrical diagnostics like the {r, s} and {r, q} plane. We found the model to mimic the nature of a Chaplygin gas type dark energy model at early times while a Quintessence type in distant future. Finally, we study the violation of continuity equation for our model and show that in order to explain the cosmic acceleration at the present epoch, energymomentum must violate.

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Bouncing scenario in f(R,T) gravity

Cited by 57 publications

References 49 publications

Inflation in f(R, T) gravity

Inflation in f(R, T) gravity

Energy Conditions in Non-minimally Coupled $f(R,T)$ Gravity

Late-time viscous cosmology in f(R, T) gravity

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