  The main objective of this article is to study the viable compact stellar
structures in non-Riemannian geometry, i.e., $f(\mathbb{Q},T)$ theory, where
$\mathbb{Q}$ defines the non-metricity and $T$ represents trace of the
stress-energy tensor. In this perspective, we consider a static spherical
metric with anisotropic matter configuration to examine the geometry of
considered compact stars. A specific model of this theory is used to derive the
explicit expressions of energy density and pressure components that govern the
relationship between matter and geometry. The unknown parameters are evaluated
by using the continuity of inner and outer spacetimes to examine the
configuration of spherical stellar structures. Physical parameters such as
fluid characteristics, energy constraints and equation of state parameters are
analyzed to examine the viability of the considered stellar objects. Further,
we use Tolman-Oppenheimer-Volkoff equation, sound speed and adiabatic index
methods to analyze the equilibrium state and stability of the proposed stellar
objects. The rigorous analysis and satisfaction of necessary conditions lead to
the conclusion that the stellar objects studied in this framework are viable
and stable.
