  We have explored a transitioning cosmic model, depicting late-time
accelerated expansion in $f(R,T^{\phi})$ theory of gravity for an isotropic and
homogeneous universe, where the trace of energy-momentum tensor $T^{\phi}$ is
the function of the self-interacting scalar field $\phi$. We have proposed an
explicit solution to the derived model by utilizing a scale factor of the
hybrid form $a(t) = t^{\alpha} e^{\beta t}$, where $\alpha$ and $\beta$ are
constants. To evaluate the best-fit values of free parameters of the suggested
model, the statistical analysis based on the Markov Chain Monte Carlo (MCMC)
method has been employed on 57 OHD points. We have described the dynamical
features of the model like energy density, cosmic pressure, and equation of
state parameter in the context of scalar field $\phi$. We have also described
the potential and behavior of the scalar field for quintessence and phantom
scenarios. The deceleration parameter depicts a transitioning universe with
signature flipping at $z_t = 0.82$ with the present value of deceleration
parameter $q_0=-0.41$. The violation of SEC for the derived model indicates the
cosmic expansion at a faster rate. We have used statefinders to diagnose the
model. The findings for our theoretical model indicate that the derived model
agrees with observed findings within a particular range of limitations.
