Preface

Alam, Aniket

doi:10.1017/upo9788175968387.001

Cited by 4 publications

(4 citation statements)

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“…where M ′ ≡ µ 0 + M is a nuisance parameter which includes the absolute magnitude and the parameter h. The nuisance parameter M ′ can be marginalized over analytically [40][41][42][43][44][45][46] as…”

Section: A Type Ia Supernovaementioning

confidence: 99%

Investigate the interaction between dark matter and dark energy

Jin

et al. 2012

Results in Physics

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In this paper we investigate the interaction between dark matter and dark energy by considering two different interacting scenarios, i.e. the cases of constant interaction function and variable interaction function. By fitting the current observational data to constrain the interacting models, it is found that the interacting strength is non-vanishing, but weak for the case of constant interaction function, and the interaction is not obvious for the case of variable interaction function. In addition, for seeing the influence from interaction we also investigate the evolutions of interaction function, effective state parameter for dark energy and energy density of dark matter. At last some geometrical quantities in the interacting scenarios are discussed.

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Section: A Type Ia Supernovaementioning

confidence: 99%

Investigate the interaction between dark matter and dark energy

Jin

et al. 2012

Results in Physics

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“…where M ′ ≡ µ 0 + M is a nuisance parameter which includes the absolute magnitude and the parameter h. The nuisance parameter M ′ can be marginalized over analytically [100][101][102][103][104][105][106] as…”

Section: Type Ia Supernovaementioning

confidence: 99%

Does accelerating universe indicate Brans-Dicke theory?

Wang

et al. 2011

Eur. Phys. J. Plus

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The evolution of universe in Brans-Dicke (BD) theory is discussed in this paper. Considering a parameterized scenario for BD scalar field φ = φ0a α which plays the role of gravitational constant G, we apply the Markov Chain Monte Carlo method to investigate a global constraints on BD theory with a self-interacting potential according to the current observational data: the Union2 dataset of type supernovae Ia (SNIa), the high-redshift Gamma-Ray Bursts (GRBs) data, the observational Hubble data (OHD), the cluster X-ray gas mass fraction, the baryon acoustic oscillation (BAO), and the cosmic microwave background (CMB) data. It is shown that an expanded universe from deceleration to acceleration is given in this theory, and the constraint results of dimensionless matter density Ω0m and parameter α are, Ω0m = 0.286 +0.037+0.050 −0.039−0.047 and α = 0.0046 +0.0149+0.0171 −0.0171−0.0206 which is consistent with the result of current experiment exploration, | α |≤ 0.132124. In addition, we use the geometrical diagnostic method, jerk parameter j, to distinguish the BD theory and the cosmological constant model in Einstein's theory of general relativity.

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“…18), we cannot clearly discern various dark energy models using these two parameters once H > 0 or q < 0. Calling for more accurate calculations regarding this issue and resulting from the improvement of observational data during the recent two decades, a new geometrical diagnostic pair for tracking the dark energy models has been proposed [71,72]. This new pair letting us to specify the characteristics of dark energy is called statefinder pair (r, s) r = ... a aH 3 = 1 +Ḧ…”

Section: The Statefinder Pairmentioning

confidence: 99%

Tsallis holographic dark energy in fractal universe

2020

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We study the cosmological consequences of interacting Tsallis holographic dark energy model in the framework of the fractal universe, in which, the Hubble radius is considered as the IR cut-off. We drive the equation of state (EoS) parameter, deceleration parameter and the evolution equation for the Tsallis holographic dark energy density parameter. Our study shows that this model can describe the current accelerating Universe in both noninteracting and interacting scenarios, and also a transition occurs from the deceleration phase to the accelerated phase, at the late time. Finally, we check the compatibility of free parameters of the model with the latest observational results by using the Pantheon supernovae data, eBOSS, 6df, BOSS DR12, CMB Planck 2015, Gamma-Ray Burst.

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Preface

Cited by 4 publications

References 0 publications

Investigate the interaction between dark matter and dark energy

Investigate the interaction between dark matter and dark energy

Does accelerating universe indicate Brans-Dicke theory?

Tsallis holographic dark energy in fractal universe

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