This paper investigates the impact of $ f(\mathcal{Q}, \mathcal{T}) $ gravity on the geometry of anisotropic compact stellar objects. The study uses physically viable non-singular solutions to examine the configuration of static spherically symmetric structures. A specific model of the theory is considered to analyze various physical quantities such as 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. The paper explores the theoretical implications, compatibility with observational data, and relevance in cosmological contexts of $ f(\mathcal{Q}, \mathcal{T}) $ gravity. It discusses how this theory changes the nature of tidal forces and the equation of motion in the Newtonian limit, suggesting deviations from classical predictions. The study also examines the formation and evolution of galaxies, the role of stars in maintaining equilibrium, and the characteristics of compact stars (CSs) such as neutron stars and pulsars. The paper analyzes the viability of CSs in $ f(\mathcal{Q}, \mathcal{T}) $ gravity using the Krori-Barua solution, which is non-singular and positively increasing. The solution is matched with an exterior geometry to ensure continuity of metric potentials. The field equations are derived and solved for specific models of $ f(\mathcal{Q}, \mathcal{T}) $ gravity, leading to expressions for energy density, radial and tangential pressures, and other physical quantities. The study examines the physical characteristics of CSs, including the behavior of matter contents, anisotropic pressure, energy conditions, equation of state parameters, mass, compactness, and redshift. It finds that the proposed CSs satisfy the necessary conditions for viability and stability, including the positivity of energy constraints, the range of equation of state parameters, and the adiabatic index. The analysis also shows that the compactness and redshift functions lie within the specified limits, ensuring the physical viability of the stars. The equilibrium and stability analysis of CSs is performed using the sound speed and adiabatic index methods. The results show that the proposed CSs are in equilibrium and stable, with the total effect of gravitational, hydrostatic, and anisotropic forces being zero. The causality condition and Herrera cracking approach confirm the stability of the stars, as the sound speed components lie within the [0,1] interval and the cracking condition is satisfied. The adiabatic index is found to be greater than 4/3, ensuring the stability of the compact stars. The study concludes that the proposed CSs are viable and stable in $ f(\mathcal{QThis paper investigates the impact of $ f(\mathcal{Q}, \mathcal{T}) $ gravity on the geometry of anisotropic compact stellar objects. The study uses physically viable non-singular solutions to examine the configuration of static spherically symmetric structures. A specific model of the theory is considered to analyze various physical quantities such as 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. The paper explores the theoretical implications, compatibility with observational data, and relevance in cosmological contexts of $ f(\mathcal{Q}, \mathcal{T}) $ gravity. It discusses how this theory changes the nature of tidal forces and the equation of motion in the Newtonian limit, suggesting deviations from classical predictions. The study also examines the formation and evolution of galaxies, the role of stars in maintaining equilibrium, and the characteristics of compact stars (CSs) such as neutron stars and pulsars. The paper analyzes the viability of CSs in $ f(\mathcal{Q}, \mathcal{T}) $ gravity using the Krori-Barua solution, which is non-singular and positively increasing. The solution is matched with an exterior geometry to ensure continuity of metric potentials. The field equations are derived and solved for specific models of $ f(\mathcal{Q}, \mathcal{T}) $ gravity, leading to expressions for energy density, radial and tangential pressures, and other physical quantities. The study examines the physical characteristics of CSs, including the behavior of matter contents, anisotropic pressure, energy conditions, equation of state parameters, mass, compactness, and redshift. It finds that the proposed CSs satisfy the necessary conditions for viability and stability, including the positivity of energy constraints, the range of equation of state parameters, and the adiabatic index. The analysis also shows that the compactness and redshift functions lie within the specified limits, ensuring the physical viability of the stars. The equilibrium and stability analysis of CSs is performed using the sound speed and adiabatic index methods. The results show that the proposed CSs are in equilibrium and stable, with the total effect of gravitational, hydrostatic, and anisotropic forces being zero. The causality condition and Herrera cracking approach confirm the stability of the stars, as the sound speed components lie within the [0,1] interval and the cracking condition is satisfied. The adiabatic index is found to be greater than 4/3, ensuring the stability of the compact stars. The study concludes that the proposed CSs are viable and stable in $ f(\mathcal{Q