Exploring the Cosmological Model in $f(R,T^{\varphi })$ Gravity with Observational Constraints

Abstract

We have investigated an isotropic and homogeneous cosmological model of the universe in $f(R,T^{\varphi })$ gravity, where $T^{\varphi }$ is the trace of the energy-momentum tensor and $R$ is the Ricci scalar. We developed and presented exact solutions of field equations of the proposed model by taking the parametrization $q(z)=\alpha +\frac{\beta z}{1+z}$, where $\alpha$ and $\beta$ are arbitrary constants. The best possible values of the model's free parameters are estimated using the latest observational data sets of OHD, BAO, and Pantheon by applying the MCMC statistical technique. Some kinematic properties like density parameter ${\rho }_{\varphi }$, pressure $p_{\varphi }$, and equation of state parameter ${\omega }_{\varphi }$ are derived. We have also discussed the behavior of the scalar potential $V(\varphi )$ in the $f(R,T^{\varphi })$ gravity theory. The behaviors of scalar fields for quintessence and phantom models are explored. Furthermore, we have discussed the behavior of energy conditions and sound speed in $f(R,T^{\varphi })$ cosmology.

18 pages, 12 figures

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