  The main objective of this paper is to investigate the impact of
$f(\mathcal{Q},\mathcal{T})$ gravity on the geometry of anisotropic compact
stellar objects, where $\mathcal{Q}$ is non-metricity and $\mathcal{T}$ is the
trace of the energy-momentum tensor. In this perspective, we use the physically
viable non-singular solutions to examine the configuration of static
spherically symmetric structures. We consider a specific model of this theory
to examine various physical quantities in the interior of the proposed compact
stars. These quantities include fluid parameters, anisotropy, energy
constraints, equation of state parameters, mass, compactness and redshift. The
Tolman-Oppenheimer-Volkoff equation is used to examine the equilibrium state of
stellar models, while the stability of the proposed compact stars is
investigated through sound speed and adiabatic index methods. It is found that
the proposed compact stars are viable and stable in the context of this theory.
