  We investigate irregularity factors for a self-gravitating spherical star
evolving in the presence of imperfect fluid. We explore the gravitational field
equations and the dynamical equations with the systematic construction in
$f(R,T)$ gravity, where $T$ is the trace of the energy-momentum tensor.
Furthermore, we analyze two well-known differential equations (which occupy
principal importance in the exploration of causes of energy density
inhomogeneities) with the help of the Weyl tensor and the conservation laws.
The irregularity factors for a spherical star are examined for particular cases
of dust, isotropic and anisotropic fluids in dissipative and non-dissipative
regimes in the framework of $f(R,T)$ gravity. It is found that as the
complexity in the matter with the anisotropic stresses increases, the
inhomogeneity factor has more correspondences to one of the structure scalars.
