This paper investigates the viability and stability of compact stellar objects with anisotropic matter in the framework of $ f(\mathbf{Q}, \mathbf{T}) $ theory, where $ \mathbf{Q} $ represents non-metricity and $ \mathbf{T} $ is the trace of the energy-momentum tensor. A specific model of this theory is considered to derive explicit expressions for the field equations governing the behavior of matter and geometry. The Karmarkar condition is employed to assess the configuration of static spherically symmetric structures. The values of unknown constants in the metric potentials are determined through matching conditions of the interior and exterior spacetimes. Various physical quantities such as fluid parameters, energy constraints, equation of state parameters, mass, compactness, and redshift are graphically analyzed to evaluate the viability of the considered compact stars. The Tolman-Oppenheimer-Volkoff equation is used to examine the equilibrium state of the stellar models. Moreover, the stability of the proposed compact stars is investigated through sound speed and adiabatic index methods. The study concludes that the proposed compact stars analyzed in this theoretical framework are viable and stable, as all the required conditions are satisfied. The $ f(\mathbf{Q}, \mathbf{T}) $ theory is employed as a mathematical tool to scrutinize obscure aspects of gravitational dynamics on a large scale. Investigations into this modified theory have extended to its implications for cosmic models and the accelerated expansion of the universe. The motivation driving the exploration of this theory encompasses an examination of its theoretical implications, its alignment with observational data, and its significance in cosmological contexts. The study of observational constraints in modified gravities has been discussed in recent literature. The above literature motivates us to investigate the viable characteristics of anisotropic compact stars in the context of $ f(\mathbf{Q}, \mathbf{T}) $ theory. We use the following format in the paper. Section 2 presents the fundamental formulation of $ f(\mathbf{Q}, \mathbf{T}) $ gravity. In section 3, a specific model of this theory is considered to derive explicit expressions for energy density and pressure components. We evaluate unknown parameters through the matching conditions. In Section 4, various physical quantities are used to determine the physical features of the considered compact stars. Furthermore, the equilibrium state and the stability of the considered compact stars are analyzed in Section 5. We compile our findings in Section 6.This paper investigates the viability and stability of compact stellar objects with anisotropic matter in the framework of $ f(\mathbf{Q}, \mathbf{T}) $ theory, where $ \mathbf{Q} $ represents non-metricity and $ \mathbf{T} $ is the trace of the energy-momentum tensor. A specific model of this theory is considered to derive explicit expressions for the field equations governing the behavior of matter and geometry. The Karmarkar condition is employed to assess the configuration of static spherically symmetric structures. The values of unknown constants in the metric potentials are determined through matching conditions of the interior and exterior spacetimes. Various physical quantities such as fluid parameters, energy constraints, equation of state parameters, mass, compactness, and redshift are graphically analyzed to evaluate the viability of the considered compact stars. The Tolman-Oppenheimer-Volkoff equation is used to examine the equilibrium state of the stellar models. Moreover, the stability of the proposed compact stars is investigated through sound speed and adiabatic index methods. The study concludes that the proposed compact stars analyzed in this theoretical framework are viable and stable, as all the required conditions are satisfied. The $ f(\mathbf{Q}, \mathbf{T}) $ theory is employed as a mathematical tool to scrutinize obscure aspects of gravitational dynamics on a large scale. Investigations into this modified theory have extended to its implications for cosmic models and the accelerated expansion of the universe. The motivation driving the exploration of this theory encompasses an examination of its theoretical implications, its alignment with observational data, and its significance in cosmological contexts. The study of observational constraints in modified gravities has been discussed in recent literature. The above literature motivates us to investigate the viable characteristics of anisotropic compact stars in the context of $ f(\mathbf{Q}, \mathbf{T}) $ theory. We use the following format in the paper. Section 2 presents the fundamental formulation of $ f(\mathbf{Q}, \mathbf{T}) $ gravity. In section 3, a specific model of this theory is considered to derive explicit expressions for energy density and pressure components. We evaluate unknown parameters through the matching conditions. In Section 4, various physical quantities are used to determine the physical features of the considered compact stars. Furthermore, the equilibrium state and the stability of the considered compact stars are analyzed in Section 5. We compile our findings in Section 6.