This paper investigates viable compact stellar structures in the context of non-Riemannian geometry, specifically within the framework of the $ f(\mathbb{Q}, T) $ theory, where $ \mathbb{Q} $ represents non-metricity and $ T $ is the trace of the stress-energy tensor. The study considers a static spherical metric with anisotropic matter distribution to examine the geometry of compact stars. The theory is applied to derive explicit expressions for energy density and pressure components that govern the relationship between matter and geometry. The unknown parameters are determined by ensuring continuity between the inner and outer spacetimes, allowing for the analysis of the configuration of spherical stellar structures. Physical parameters such as fluid characteristics, energy constraints, and equation of state parameters are analyzed to assess the viability of the considered stellar objects. The Tolman-Oppenheimer-Volkoff equation, sound speed, and adiabatic index methods are employed to analyze the equilibrium and stability of the proposed stellar objects. The rigorous analysis and satisfaction of necessary conditions confirm that the stellar objects studied in this framework are viable and stable. The paper reviews existing literature on non-Riemannian geometries, including theories like $ f(\mathbb{Q}) $ gravity, which extend Riemannian geometry to describe spacetime curvature with torsion or non-metricity. These theories have been studied for their theoretical implications, compatibility with observational data, and significance in cosmological contexts. The $ f(\mathbb{Q}, T) $ theory introduces the trace of the stress-energy tensor into the functional action, modifying the internal structure of compact stars and influencing the relationship between pressure and density, as well as stellar radii and mass profiles. The study uses specific models of the $ f(\mathbb{Q}, T) $ theory to analyze the physical characteristics of compact stars, including energy density, radial and tangential pressures, anisotropy, and energy bounds. The results show that the proposed stellar objects are physically viable, with all energy constraints satisfied. The analysis of the equation of state parameters confirms that the radial and transverse parameters lie within the required range for a viable model. The stability analysis of the stars is conducted using the Tolman-Oppenheimer-Volkoff equation, sound speed, and adiabatic index. The results indicate that the stars are in equilibrium, with the total effect of all forces being zero. The sound speed components and adiabatic index also confirm the stability of the proposed stellar objects, as they satisfy the necessary constraints. In conclusion, the study demonstrates that the $ f(\mathbb{Q}, T) $ theory provides a viable framework for understanding compact stellar structures, with the stars being stable and physically viable under the given conditions. The results contribute to the broader understanding of gravity and the behavior of compact stars in modified gravitational theories.This paper investigates viable compact stellar structures in the context of non-Riemannian geometry, specifically within the framework of the $ f(\mathbb{Q}, T) $ theory, where $ \mathbb{Q} $ represents non-metricity and $ T $ is the trace of the stress-energy tensor. The study considers a static spherical metric with anisotropic matter distribution to examine the geometry of compact stars. The theory is applied to derive explicit expressions for energy density and pressure components that govern the relationship between matter and geometry. The unknown parameters are determined by ensuring continuity between the inner and outer spacetimes, allowing for the analysis of the configuration of spherical stellar structures. Physical parameters such as fluid characteristics, energy constraints, and equation of state parameters are analyzed to assess the viability of the considered stellar objects. The Tolman-Oppenheimer-Volkoff equation, sound speed, and adiabatic index methods are employed to analyze the equilibrium and stability of the proposed stellar objects. The rigorous analysis and satisfaction of necessary conditions confirm that the stellar objects studied in this framework are viable and stable. The paper reviews existing literature on non-Riemannian geometries, including theories like $ f(\mathbb{Q}) $ gravity, which extend Riemannian geometry to describe spacetime curvature with torsion or non-metricity. These theories have been studied for their theoretical implications, compatibility with observational data, and significance in cosmological contexts. The $ f(\mathbb{Q}, T) $ theory introduces the trace of the stress-energy tensor into the functional action, modifying the internal structure of compact stars and influencing the relationship between pressure and density, as well as stellar radii and mass profiles. The study uses specific models of the $ f(\mathbb{Q}, T) $ theory to analyze the physical characteristics of compact stars, including energy density, radial and tangential pressures, anisotropy, and energy bounds. The results show that the proposed stellar objects are physically viable, with all energy constraints satisfied. The analysis of the equation of state parameters confirms that the radial and transverse parameters lie within the required range for a viable model. The stability analysis of the stars is conducted using the Tolman-Oppenheimer-Volkoff equation, sound speed, and adiabatic index. The results indicate that the stars are in equilibrium, with the total effect of all forces being zero. The sound speed components and adiabatic index also confirm the stability of the proposed stellar objects, as they satisfy the necessary constraints. In conclusion, the study demonstrates that the $ f(\mathbb{Q}, T) $ theory provides a viable framework for understanding compact stellar structures, with the stars being stable and physically viable under the given conditions. The results contribute to the broader understanding of gravity and the behavior of compact stars in modified gravitational theories.