Emergent Universe from a composition of matter, exotic matter and dark energy

Paul, Bikash Chandra; Ghose, Subrata; Thakur, P.

doi:10.1111/j.1365-2966.2010.18177.x

Cited by 40 publications

(37 citation statements)

References 27 publications

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“…Recently, H ( z ) data at 11 different redshifts based on the differential ages of red‐envelope galaxies were reported by Stern et al (2010) while three more H ( z ) data points were obtained by Gaztanaga, Cabre & Hui (2009). The newly obtained H ( z ) data points have been used to constrain parameters of various cosmological models (Paul, Thakur & Ghose 2010; Yang & Zhang 2010; Cao, Zhu & Liang 2011; Chen & Ratra 2011; Paul, Ghose & Thakur 2011). Here, we use 13 observational H ( z ) data points given in table 1 of Chen & Ratra (2011) and the one at z = 0 estimated in the work by Riess et al (2011).…”

Section: Constraints From Observational Hz Datamentioning

confidence: 99%

Observational constraints on Hubble constant and deceleration parameter in power-law cosmology

Kumar

2012

Monthly Notices of the Royal Astronomical Society

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In this paper, we show that the expansion history of the Universe in power‐law cosmology essentially depends on two crucial parameters, namely the Hubble constant H0 and deceleration parameter q. We find the constraints on these parameters from the latest H(z) and SNe Ia data. At 1σ level the constraints from H(z) data are obtained as and km s−1 Mpc−1, while the constraints from the Type Ia supernovae (SNe Ia) data are and km s−1 Mpc−1. We also perform the joint test using H(z) and SNe Ia data, which yields the constraints and km s−1 Mpc−1. The estimates of H0 are found to be in close agreement with some recent probes carried out in the literature. The analysis reveals that the observational data successfully describe the cosmic acceleration within the framework of power‐law cosmology. We find that the power‐law cosmology accommodates well the H(z) and SNe Ia data. We also test the power‐law cosmology using the primordial nucleosynthesis, which yields the constraints q≳ 0.72 and H0≲ 41.49 km s−1 Mpc−1. These constraints are found to be inconsistent with the ones derived from the H(z) and SNe Ia data. We carry out the statefinder analysis, and find that the power‐law cosmological models approach the standard Λ cold dark matter (ΛCDM) model as q→−1. Finally, we conclude that despite having several good features power‐law cosmology is not a complete package for the cosmological purposes.

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Section: Constraints From Observational Hz Datamentioning

confidence: 99%

Observational constraints on Hubble constant and deceleration parameter in power-law cosmology

Kumar

2012

Monthly Notices of the Royal Astronomical Society

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“…This model (2.1) can produce a emergent universe without the time singularity [43][44][45][46]. But in this paper, we will take this RMCG fluid as the dark components in our Universe.…”

Section: Dark Models In Rmcg Cosmologymentioning

confidence: 99%

Reduced modified Chaplygin gas cosmology

Geng

et al. 2015

J. High Energ. Phys.

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Abstract:In this paper, we study cosmologies containing the reduced modified Chaplygin gas (RMCG) fluid which is reduced from the modified Chaplygin gas p = Aρ − Bρ −α for the value of α = −1/2. In this special case, dark cosmological models can be realized for different values of model parameter A. We investigate the viabilities of these dark cosmological models by discussing the evolutions of cosmological quantities and using the currently available cosmic observations. It is shown that the special RMCG model (A = 0 or A = 1) which unifies the dark matter and dark energy should be abandoned. For A = 1/3, RMCG which unifies the dark energy and dark radiation is the favorite model according to the objective Akaike information criteria. In the case of A < 0, RMCG can achieve the features of the dynamical quintessence and phantom models, where the evolution of the universe is not sensitive to the variation of model parameters.

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“…The parameter K , however, appears in the theory as an integration constant and may be fixed to some other value for a different initial configuration. Paul, Ghose & Thakur (2011) recently worked with a more specific model for a small value of A ( A ≈ 0). In the original work of Mukherjee et al (2006) it was shown that the choice of A drastically changes the matter energy composition of the universe that can mimic.…”

Section: Introductionmentioning

confidence: 99%