Modified Chaplygin gas in Horava-Lifshitz gravity and constraints on its<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>B</mml:mi></mml:math>parameter

Paul, Bikash Chandra; Thakur, P.; Saha, Arindam

doi:10.1103/physrevd.85.024039

Cited by 18 publications

(23 citation statements)

References 39 publications

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“…Assuming A 2 = 0 gives MCG [76], while A 2 = A 1 = 0 gives GCG [75] where A 1 , B, and α are positive constants with 0 < α ≤ 1. Therefore, we have four free parameters in our model.…”

Section: Extended Chaplygin Gasmentioning

confidence: 99%

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Extended Chaplygin gas in Horava–Lifshitz gravity

Pourhassan

2016

Physics of the Dark Universe

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In this paper, we investigate cosmological models of the extended Chaplygin gas in a universe governed by Horava-Lifshitz gravity. The equation of state for an extended Chaplygin gas is a (n + 2)-variable equation determined by A n , α, and B. In this work, we are interested to the case of second order (n = 2) equation of state which recovers quadratic barotropic equation of state. In that case there are four free parameters. We solve conservation equation approximately and obtain energy density in terms of scale factor with mentioned free parameters. Under some assumptions we relate free parameters to each other to have only one free independent parameter (A 2 ). It help us to obtain explicit expression for energy density in terms of scale factor. The allowed values of the second order extended Chaplygin gas parameter is fixed using the recent astrophysical and cosmological observational data. Thermodynamics of the model investigated based on the first and second law of thermodynamics.

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“…Assuming A 2 = 0 gives MCG [76], while A 2 = A 1 = 0 gives GCG [75] where A 1 , B, and α are positive constants with 0 < α ≤ 1. Therefore, we have four free parameters in our model.…”

Section: Extended Chaplygin Gasmentioning

confidence: 99%

“…Also, MCG in HL gravity and observational constraints has been studied by the Refs. [76,77] with possibility of extension to the case of varying G and Λ [78]. Now, we would like to investigate ECG in HL gravity.…”

Section: Contents 1 Introductionmentioning

confidence: 99%

Extended Chaplygin gas in Horava–Lifshitz gravity

Pourhassan

2016

Physics of the Dark Universe

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“…where K = −1, 1, 0 represent open, closed and flat universe respectively and taking variation of N and g ij we obtain the Friedmann equations [14,30] …”

Section: Basic Equations In Horava-lifshitz Gravitymentioning

confidence: 99%

“…Park himself considered the widely used CPL parametrization. B. C. Paul and his coleagues have studied constraints for different exotic fluid model in the back ground of HL gravity [29,30]. In this work, we shall study the limits of the DE parameters constrained by different data sets.…”

Section: Introductionmentioning

confidence: 99%

Observational Data Fitting to Constrain Variable Modified Chaplygin Gas in the Background of Horava-Lifshitz Gravity

Ranjit¹,

Rudra²

2015

Int J Theor Phys

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FRW universe in Horava-Lifshitz (HL) gravity model filled with a combination of dark matter and dark energy in the form of variable modified Chaplygin gas (VMCG) is considered. The permitted values of the VMCG parameters are determined by the recent astrophysical and cosmological observational data. Here we present the Hubble parameter in terms of the observable parameters Ω dm0 , Ω vmcg0 , H 0 , redshift z and other parameters like α, A, γ and n. From Stern data set (12 points), we have obtained the bounds of the arbitrary parameters by minimizing the χ 2 test. The best-fit values of the parameters are obtained by 66%, 90% and 99% confidence levels. Next due to joint analysis with BAO and CMB observations, we have also obtained the bounds of the parameters (A, γ) by fixing some other parameters α and n. The best fit value of distance modulus µ(z) is obtained for the VMCG model in HL gravity, and it is concluded that our model is perfectly consistent with the union2 sample data.Pacs no : 04.60. Pp, 98.80.Qc,

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“…This model incorporates an extra parameter which is associated to a lower bound on the sound speed of the effective DM component. The MCG has been observationally constrained using the redshift dependence of the apparent magnitude of type Ia supernovae, the Cosmic Microwave Background (CMB) anisotropies, and the matter power spectrum, including Baryonic Acoustic Oscillations (BAO) [25][26][27][28][29][30][31][32][33][34]. Further extensions incorporating additional terms accounting for a possible growth of the comoving Jeans length with cosmic density have also been proposed in the literature (see, e.g., [35]).…”

Section: Introductionmentioning

confidence: 99%

Constraints on the dark matter sound speed from galactic scales: The cases of the modified and extended Chaplygin gas

Avelino¹,

Ferreira²

2015

Phys. Rev. D

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We show that the observed rotation curves of spiral galaxies constrain the sound speed of the dark matter to be cs < 10 −4 c, where c is the speed of light in vacuum. Using the Modified Chaplygin Gas as a representative example of a class of unified dark energy models incorporating an effective dark matter component with a non-zero sound speed, we determine the most stringent constraint to date on the value of the constant contribution to the equation of state parameter in this class of models. Finally, we explain the reason why previous constraints using the Cosmic Microwave Background and Baryonic Acoustic Oscillations were not as competitive as the one presented in this paper and discuss the limitations of the recently proposed Extended Chaplygin Gas.

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Modified Chaplygin gas in Horava-Lifshitz gravity and constraints on itsBparameter

Cited by 18 publications

References 39 publications

Extended Chaplygin gas in Horava–Lifshitz gravity

Extended Chaplygin gas in Horava–Lifshitz gravity

Observational Data Fitting to Constrain Variable Modified Chaplygin Gas in the Background of Horava-Lifshitz Gravity

Constraints on the dark matter sound speed from galactic scales: The cases of the modified and extended Chaplygin gas

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