Abstract
An exact cosmological solution of Einstein’s field equations (EFEs) is derived for a dynamical vacuum energy in f(R, T) gravity for Friedmann–Lemaitre–Robertson–Walker (FLRW) space-time. A parametrization of the Hubble parameter is used to find a deterministic solution of the EFE. The cosmological dynamics of our model is discussed in detail. We have analyzed the time evolution of the physical parameters and obtained their bounds analytically. Moreover, the behavior of these parameters are shown graphically in terms of the redshift ‘z’. Our model is consistent with the formation of structure in the Universe. The role of the f(R, T) coupling constant lambda is discussed in the evolution of the equation of state parameter. The statefinder and Om diagnostic analysis is used to distinguish our model with other dark energy models. The maximum likelihood analysis has been reviewed to obtain the constraints on the Hubble parameter H_0 and the model parameter n by taking into account the observational Hubble data set H(z), the Union 2.1 compilation data set SNeIa, the Baryon Acoustic Oscillation data BAO, and the joint data set H(z) + mathrm{SNeIa} and H(z) + mathrm{SNeIa} + mathrm{BAO} . It is demonstrated that the model is in good agreement with various observations.
Highlights
The two main models proposed in the literature to explain the nature of dark energy (DE) are the model of the cosmological constant, i.e. assuming a constant energy density filling in space homogeneously, and a scalar field model, which considers a dynamical variable energy density in space-time
We have presented a (t) cosmology model obtained by a simple parametrization of the Hubble parameter in a flat Friedmann–Lemaitre– Robertson–Walker (FLRW) space-time in f (R, T ) modified gravity theory
We have studied the most simple form of f (R, T ) function that can explain the non-minimal coupling between geometry and matter present in the Universe
Summary
The two main models proposed in the literature to explain the nature of DE are the model of the cosmological constant , i.e. assuming a constant energy density filling in space homogeneously, and a scalar field model, which considers a dynamical variable energy density in space-time. Shabani et al have discussed the cosmological and solar system consequences of a non-interacting generalized Chaplygin gas (GCG) with baryonic matter, late-time solutions of the CDM subclass of f (R, T ) gravity using a dynamical system approach, latetime cosmological evolution of the Universe in f (R, T ) gravity with minimal curvature–matter coupling via considering linear perturbations in the neighborhood of equilibrium, and bouncing cosmological models against the background of f (R, T ) = R + h(T ) gravity in FLRW metric with a perfect fluid [66,67,68,69,70,71].
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