Effect of Shear and Bulk Viscosities on Interacting Modified Chaplygin Gas Cosmology

Naji, J.; Pourhassan, B.; Amani, Alireza

doi:10.1142/s0218271814500205

Cited by 52 publications

(37 citation statements)

References 31 publications

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“…where Q is the interaction term between the dark energy and modified Chaplygin gas, that one be usually considered as: Q = 3Hb 2 ρ DE , Q = 3Hb 2 ρ M CG and Q = 3Hb 2 ρ tot in which b 2 is the coupling parameter or transfer strength [23,24,46,52,53]. This choice is based on positive motivation Q, because from the observational data at the four years W M AP implies that the coupling parameter must be a small positive value [8,54].…”

Section: Fundamental Of F (R T ) Gravitymentioning

confidence: 99%

“…As we discussed, the acceleration can be consequence of the dark energy influence that this leads to some other models called Chaplygin gas [13,24,[43][44][45][46]. Chaplygin gas is a fluid with negative pressure that begins to dominate the matter content and, at the end, the process of structure formation is driven by cold dark matter without affecting the previous history of the universe.…”

Section: Introductionmentioning

confidence: 98%

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Interacting F(R, T) gravity with modified Chaplygin gas

Amani

2015

Can. J. Phys.

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In this paper, we have studied F (R, T ) gravity as an arbitrary function of curvature and torsion scalars in Friedmann-Lemaître-Robertson-Walker (FLRW) background. Then, we have considered interacting model between F (R, T ) gravity and modified Chaplygin gas. The novelty of this model is that the Universe includes both cases curvature and torsion, and one dominated by a Chaplygin gas. In order to calculate cosmological solutions, we obtained Friedmann equations and also equation of state (EoS) parameter of dark energy. By employing interacting model we considered the total energy density and the total pressure of Universe as the combination of components of dark energy and Chaplygin gas. Subsequently, we reconstructed the model by an origin of a scalar field entitled quintessence model with a field potential. The field potential has been calculated in terms of free parameters of F (R, T ) gravity and modified Chaplygin gas. In what follows, we used a parametrization, and the cosmological parameters have been written in terms of redshift z. Next, we plotted cosmological parameters with respect to three variable of cosmic time, redshift z and e-folding number N = ln(a), and the figures showed us an accelerated expansion of Universe. Also, we have described the scenario in three status early time, late time and future time by e-folding number. Finally, the stability of scenario has been investigated by a useful function named sound speed, and the graph of sound speed versus e-folding number has been showed us that there is the stability in late time.PACS numbers: 04.50.Kd; 95.36.+x

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Section: Fundamental Of F (R T ) Gravitymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 98%

Interacting F(R, T) gravity with modified Chaplygin gas

Amani

2015

Can. J. Phys.

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“…It is also possible to consider viscosity in above models [15][16][17][18][19][20][21][22][23][24][25]. Another way to study dark energy arises from holographic principle states that the number of degrees of freedom related directly to the entropy scales with the enclosing area of the system.…”

Section: +007mentioning

confidence: 99%

Interacting holographic extended Chaplygin gas and phantom cosmology in the light of BICEP2

2015

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Abstract:In this paper, we study the holographic dark energy density and interacting extended Chaplygin gas energy density in the Einstein gravity. We reconstruct the scalar field and the scalar potential describing the extended Chaplygin gas. In the special case, we obtain energy density and investigate some cosmological parameters. Assuming interaction between components we find energy density for some different parametrization of total EoS. We analyze tensor to scalar ratio and use recent observational data of BICEP2 to fix the model parameters.

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“…In order to describe dark energy model, numerous studies have been performed in isotropic space-time such as scalar fields (quintessence, phantom, tachyon and etc.) [6][7][8][9][10][11][12][13][14][15][16][17][18][19][20][21][22][23], modified gravity models [24][25][26][27][28][29][30][31], holographic models [32][33][34][35][36][37][38][39][40], interacting models [41][42][43][44][45][46][47][48][49][50][51][52], bouncing model [53][54][55...…”

Section: Introductionnmentioning

confidence: 99%

Stability and interacting f(T, T ) gravity with modified Chaplygin gas

Rezaei

Amani

2017

Can. J. Phys.

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In this paper, the model of interaction is studied between f (T, T ) gravity and modified Chaplygin gas in FRW-flat metric. We obtain the Friedmann equations in the framework of teleparallel gravity by vierbein field. We consider that Universe dominates by components of cold matter, dark energy and modified Chaplygin gas. In what follows we separately write the corresponding continuity equations for components of Universe. Also, dark energy EoS and effective EoS are obtained with respect to redshift, thereafter the corresponding cosmological parameters are plotted in terms of redshift, thereinafter the accelerated expansion of the Universe is investigated. Finally, the stability of the model is discussed in phase plane analysis.PACS numbers: 98.80.-k; 95.36.+x; 95.35.+d

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Effect of Shear and Bulk Viscosities on Interacting Modified Chaplygin Gas Cosmology

Cited by 52 publications

References 31 publications

Interacting F(R, T) gravity with modified Chaplygin gas

Interacting F(R, T) gravity with modified Chaplygin gas

Interacting holographic extended Chaplygin gas and phantom cosmology in the light of BICEP2

Stability and interacting f(T, T ) gravity with modified Chaplygin gas

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