A Dark Energy Model with Generalized Uncertainty Principle in the Emergent, Intermediate and Logamediate Scenarios of the Universe

Ghosh, Rahul; Chattopadhyay, Surajit; Debnath, Ujjal

doi:10.1007/s10773-011-0939-z

Cited by 16 publications

(9 citation statements)

References 60 publications

(117 reference statements)

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“…This form of scale factor a (t), as stated in [67][68][69] is given by: gravity theory: they derived that this model is able to lead to a stable past eternal static solution which eventually is able to enter a phase where the stability is broken, which leads to a period of inflation.…”

Section: Scale Factor Pertaining To Emergent Scenariomentioning

confidence: 99%

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Consequences of three modified forms of holographic dark energy models in bulk–brane interaction

Pasqua

Chattopadhyay²,

Myrzakulov

2018

Can. J. Phys.

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In this paper, we study the effects which are produced by the interaction between a brane Universe and the bulk in which the Universe is embedded. Taking into account the effects produced by the interaction between a brane Universe and the bulk, we derived the Equation of State (EoS) parameter ω D for three different models of Dark Energy (DE), i.e. the Holographic DE (HDE) model with infrared (IR) cut-off given by the Granda-Oliveros cutoff, the Modified Holographic Ricci DE (MHRDE) model and a DE model which is function of the Hubble parameter H squared and to higher derivatives of H. Moreover, we have considered two different cases of scale factor (namely, the power law and the emergent ones).A nontrivial contribution of the DE is observed to be different from the standard matter fields confined to the brane. Such contribution has a monotonically decreasing behavior upon the evolution of the Universe for the emergent scenario of the scale factor, while monotonically increasing for the power-law form of the scale factor a(t).

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Section: Scale Factor Pertaining To Emergent Scenariomentioning

confidence: 99%

“…This form of scale factor a (t), as stated in [67][68][69] is given by: where a 0 , λ , µ and m represents four positive constant parameters. We can make some considerations about the values which can be assumed by the parameters present in Eq.…”

Section: Scale Factor Pertaining To Emergent Scenariomentioning

confidence: 99%

Consequences of three modified forms of holographic dark energy models in bulk–brane interaction

Pasqua

Chattopadhyay²,

Myrzakulov

2018

Can. J. Phys.

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“…One coupling mechanism can be formally introduced into the Friedmann equations by defining an homogeneous interacting term Q(t) in the following form [8]:…”

Section: B (2+1)-frw Cosmologies With a Mixture Of Non-interacting El...mentioning

confidence: 99%

Radiation in (2+1)-dimensions

Cataldo,

García

2014

Preprint

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In this paper we discuss the radiation equation of state p = ρ/2 in (2+1)-dimensions. In (3+1)dimensions the equation of state p = ρ/3 may be used to describe either actual electromagnetic radiation (photons) as well as a gas of massless particles in a thermodynamic equilibrium (for example neutrinos). In this work it is shown that in the framework of (2+1)-dimensional Maxwell electrodynamics the radiation law p = ρ/2 takes place only for plane waves, i.e. for E = B. Instead of the linear Maxwell electrodynamics, to derive the (2+1)-radiation law for more general cases with E = B, one has to use a conformally invariant electrodynamics, which is a 2+1-nonlinear electrodynamics with a trace free energy-momentum tensor, and to perform a volumetric spatial average of the corresponding Maxwell stress-energy tensor with its electric and magnetic components at a given instant of time t.

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“…(58) and (60) is the same solution given by Eqs. ( 30)- (33). They are connected by the relation κC 2 = 3A 2 .…”

Section: A Procedures For Finding the Scalar Field As Function Of The...mentioning

confidence: 99%

Canonical and phantom scalar fields as an interaction of two perfect fluids

Cataldo

Arevalo

Mella

2013

Astrophys Space Sci

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In this article we investigate and develop specific aspects of Friedmann-Robertson-Walker (FRW) scalar field cosmologies related to the interpretation that canonical and phantom scalar field sources may be interpreted as cosmological configurations with a mixture of two interacting barotropic perfect fluids: a matter component ρ1(t) with a stiff equation of state (p1 = ρ1), and an "effective vacuum energy" ρ2(t) with a cosmological constant equation of state (p2 = −ρ2). An important characteristic of this alternative equivalent formulation in the framework of interacting cosmologies is that it gives, by choosing a suitable form of the interacting term Q, an approach for obtaining exact and numerical solutions. The choice of Q merely determines a specific scalar field with its potential, thus allowing to generate closed, open and flat FRW scalar field cosmologies.

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A Dark Energy Model with Generalized Uncertainty Principle in the Emergent, Intermediate and Logamediate Scenarios of the Universe

Cited by 16 publications

References 60 publications

Consequences of three modified forms of holographic dark energy models in bulk–brane interaction

Consequences of three modified forms of holographic dark energy models in bulk–brane interaction

Radiation in (2+1)-dimensions

Canonical and phantom scalar fields as an interaction of two perfect fluids

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