Viscous FRW Models With Particle Creation in Early Universe

Singh, C. P.

doi:10.1142/s0217732312500708

Cited by 11 publications

(3 citation statements)

References 38 publications

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“…[50] presented the evolution of the universe for inflationary, radiation and matter dominated phase by considering "gamma-law" EOS p = (γ − 1)ρ, where γ is a function of the scale factor R. Also Carvalho [51] has studied Robertson-Walker (RW) models in general relativity by assuming that the adiabatic parameter γ varies with cosmic time and presented unified description of early evolution of the universe in which an inflationary phase is followed by the radiation dominated phase. Singh and his collaborators [52,53,54,55,56] discussed FLRW model by using the variable adiabatic parameter γ as a function R and also studied the evolution of the universe as it goes from an inflationary phase to a radiation dominated phase. All these treatments therefore suggest that instead of a pure constant one can assume γ as a variable throughout the history of the universe.…”

Section: Introductionmentioning

confidence: 99%

FLRW viscous cosmological models

Khadekar,

Ray,

Meng

2016

Preprint

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In this paper we solve Friedmann equations by considering a universal media as a non-perfect fluid with bulk viscosity and is described by a general "gamma law" equation of state of the form p = (γ − 1)ρ + Λ(t), where the adiabatic parameter γ varies with scale factor R of the metric and Λ is the time dependent cosmological constant. A unified description of the early evolution of the universe is presented by assuming the bulk viscosity and cosmological parameter in a linear combination of two terms of the form:, where Λ 0 , Λ 1 , ζ 0 and ζ 1 are constants, in which an inflationary phase is followed by the radiation dominated phase. For this general gamma law equation of state, an entirely integrable dynamical equation to the scale factor R is obtained along with its exact solutions. In this framework we demonstrate that the model can be used to explain the dark energy dominant universe and for a special choice of the parameters we can explain the accelerating expansion of the universe also for two different phases, viz. combination of dark energy and dark matter phase as well as unified dark energy phase. A special physical check has been performed through sound speed constraint to validate the model. At last we obtain a scaling relation between the Hubble parameter with redshift.

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Section: Introductionmentioning

confidence: 99%

FLRW viscous cosmological models

Khadekar,

Ray,

Meng

2016

Preprint

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“…Also he has suggested some definitive tests that distinguish between BSCC and GR. Barber's Self Creation Cosmology has generated a lot of interest in recent times and has been widely studied [64,65,66,67,68].…”

Section: Introductionmentioning

confidence: 99%

Cosmic acceleration and anisotropic models with magnetic field

Tripathy

Mahanta

2015

Eur. Phys. J. Plus

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Plane symmetric cosmological models are investigated with or without any dark energy components in the field equations. Keeping an eye on the recent observational constraints concerning the accelerating phase of expansion of the universe, the role of magnetic field is assessed. In the absence of dark energy components, magnetic field can favour an accelerating model even if we take a linear relationship between the directional Hubble parameters. In presence of dark energy components in the form of a time varying cosmological constant, the influence of magnetic field is found to be limited.

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“…Qiang et al 49 studied a model with adiabatic particle creation which is also consistent with SNe Ia data. Singh and Beesham 50,51 , and Singh 52,53 studied early universe in FRW cosmology with particle creation through some kinematical tests. This theoretical formulation of continuous creation of matter in the universe may reinterpret several predictions of the standard Big Bang cosmology.…”

Section: Introductionmentioning

confidence: 99%

India and the Universal Periodic Review, 2012

Singh

2013

Journal of National Law University Delhi

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The theoretical and observational consequences of thermodynamics of open systems, which allow particle creation are investigated in modified f (R, T ) (R is the Ricci scalar and T is the trace of energy-momentum tensor) theory of gravity within the framework of a flat Friedmann-Robertson-Walker line element. A simplest particular model f (R, T ) = R+2f (T ) and "gamma-law" equation of state p = (γ − 1)ρ are assumed to explore the role of particle creation in the early and late time evolution of the universe. A power-law expansion model is proposed for 0 ≤ γ ≤ 2 by considering the natural phenomenological particle creation rate ψ = 3βnH, where β is a pure number of the order of unity. A Big Rip singularity is observed for γ < 0, which describes the phantom cosmology. We observe that the accelerated expansion of the universe is driven by the particle creation without any exotic "quintessence" component or a cosmological constant. It is also found by density parameter that the model becomes of negative curvature due to particle creation and the entropy increases with the evolution of the universe. Some kinematics tests such as lookback time, luminosity distance, proper distance, angular diameter versus redshift are discussed in detail to observe the role of particle creation in early and late time evolution of the universe.

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Viscous FRW Models With Particle Creation in Early Universe

Cited by 11 publications

References 38 publications

FLRW viscous cosmological models

FLRW viscous cosmological models

Cosmic acceleration and anisotropic models with magnetic field

India and the Universal Periodic Review, 2012

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