Abstract
This paper is devoted to study the cosmological behavior of homogeneous and isotropic universe model in the context of f(R,Tφ) gravity, where φ is the scalar field. For this purpose, we follow the first-order formalism defined by H=W(φ). We evaluate Hubble parameter, effective equation of state parameter (ωeff), deceleration parameter, and potential of scalar field for three different values of W(φ). We obtain phantom era in some cases for the early times. It is found that exponential expression of W(φ) yields ωeff independent of time for flat universe and independent of model parameter otherwise. It is concluded that our model corresponds to ΛCDM for both initial and late times.
Highlights
The most striking and fascinating area in cosmology is the current accelerated expansion of the universe suggested by various observations
This paper investigates the cosmological behavior of FRW universe model in the background of f(R, Tφ) gravity and in the absence of matter
We studied flat (k = 0), spherical (k = 1), and hyperbolic (k = −1) universe models assuming different values of Hubble parameter as a function of scalar field φ
Summary
The most striking and fascinating area in cosmology is the current accelerated expansion of the universe suggested by various observations. The huge difference between the vacuum energy density and the ground state energy suggested by quantum field theory leads to the first issue For this model, the densities of dark matter and dark energy are of the same order leading to cosmological coincidence problem. Nunes and Mimoso [23] worked on phase-plane analysis for a flat FRW model in the presence of perfect fluid as well as self-interacting scalar field. Moraes and Santos [27] presented a cosmological picture in f(R, Tφ) gravity in the absence of matter by considering flat FRW model They started with the relation φ = −dW/dφ which comes from the field equations of GR via the abovementioned formalism.
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