Holographic Dark Energy and Dark Matter Interaction in Anisotropic Bianchi Type-V Universe

In this study, we consider an holographic dark energy and dark matter interacting model in the Bianchi Type-V universe with a stretched exponential scale factor. We obtain the Hubble, shear, deceleration, and equation of state parameters based on the presented model and give the numerical solutions. We show that the anisotropy in the early universe plays an important role in the time evolution of the universe. Furthermore, we show that an interacting anisotropic model with stretched exponential scale factors can explain all epochs of the universe.

Probing kinematics and fate of Bianchi type V Universe

In this paper, we have constrained the cosmological parameters of Bianchi type V universe by bounding the model under consideration with recent observational [Formula: see text] and Pantheon data. It is assumed that the energy conservation law holds separately for barotropic fluid and dark energy fluid i.e. dark energy component does not interact with barotropic matter. We obtain the present value of deceleration parameter and age of universe as [Formula: see text] and 13.329 Gyrs respectively. The analysis of [Formula: see text] and jerk parameters concur that the derived model approaches [Formula: see text]CDM universe at late time. We find that estimated values of Hubble’s constant and energy density parameters have pretty consistency with their corresponding values, obtained by recent observations of WMAP and PLANCK collaborations. It is also observed that the universe shows signature flipping from decelerating to accelerating phase for transitional red-shift value [Formula: see text] in past.

Viability of Bianchi type V universe in f(R,T) = f1(R) + f2(R)f3(T) gravity

In this paper, we examine the viability of Bianchi type V universe in [Formula: see text] theory of gravitation. To solve the field equations, we have considered the power law for scale factor and constructed a singular Lagrangian model which is based on the coupling between Ricci scalar [Formula: see text] and trace of energy–momentum tensor [Formula: see text]. We find the constraints on Hubble constant [Formula: see text] and free parameter [Formula: see text] with 46 observational Hubble dataset and obtain pretty satisfactory results. The physical features of the model and transitional behavior of equation of state (EOS) parameter are analyzed. We examine the nature of physical parameters and validity of energy conditions as well as stability condition. We also present the Om[Formula: see text] and statefinder diagnostic analysis for the derived model.

Bianchi Type V Universe and Bulk Viscous Models with Time Dependent Gravitational Constant and Cosmological Constant in General Relativity

This paper deals with Bulk Viscous Models and Bianchi type- universe in the standard general relativity theory by assuming where constants, is the density. Einstein field equations ( ) have been solved in the presence of a variable gravitational constant as well as a variable cosmological constant together with a bulk viscous fluid. In order to find a deterministic solution of EFEs, a simple form of Hubble parameter being constant when where has been considered here that shows the signature flip from early deceleration to present acceleration. Moreover, the bulk viscous coefficient is allowed to vary with the density as . The physical and geometrical behavior are described in detail for the obtained model. The model obtained here is in good agreement with the present cosmological observations.

Domain walls and quark matter in Bianchi type-V universe with observational constraints in F(R,T) gravity

In this study, we investigate the Bianchi type-V cosmological models with quark matter (QM) distribution and domain walls with observational constraints in [Formula: see text] theory of gravity (Harko et al. in Phys. Rev. D 84 (2011) 024020), for a specific choice of the function [Formula: see text] (where [Formula: see text] is Ricci scalar and [Formula: see text] is the trace of the energy–momentum tensor). We have used model-independent methods and hyperbolic expansion scale factors to achieve the deterministic solution of the modified Einstein field equations and these are also tested observationally. The behaviors of QM and domain walls give an idea of accelerated expansion of the Universe which agrees with recent observations of Type Ia Supernovae. We also discuss the physical implications of the derived models.

Bianchi type-V modified holographic Ricci dark energy models in Saez–Ballester theory of gravitation

We have investigated Bianchi type-V universe filled with matter and modified holographic Ricci dark energy in a scalar–tensor theory proposed by Saez–Ballester (Phys. Lett. A, 113, 467 (1986)). To get a determinate solution, we have used (i) hybrid expansion law (Akarsu et al. JCAP, 01, 022 (2014)), (ii) varying deceleration parameter (Mishra et al. Int. J. Theor. Phys. 52, 2546 (2013)), and (iii) linearly varying deceleration parameter (Akarsu and Dereli. Int. J. Theor. Phys. 51, 612 (2012)). The various physical and geometrical aspects of the models are also discussed.

LRS Bianchi type-V universe with variable modified Chaplygin gas in a scalar–tensor theory of gravitation

The spatially homogeneous and anisotropic LRS Bianchi type-V Universe filled with variable modified Chaplygin gas in the framework of the Brans–Dicke (Brans and Dicke. Phys. Rev. 124, 925 (1961). doi:10.1103/PhysRev.124.925) scalar–tensor theory of gravitation has been studied. To obtain a determinate solution of the field equations we have used the condition that scalar field ([Formula: see text]) is a function of average scale factor. Some physical and kinematical properties of the model are discussed. We have also analyzed the stability of the solution.