Modeling Stellar Interiors via Gravitational Decoupling Approach in Non-Metricity-Matter Coupled Gravity

This article mainly aims to analyze anisotropic spherical solutions admitting minimal geometric deformation technique in the background of f ( Q , L m ) theory, where Q is the non-metricity scalar characterizing gravitational interaction and L m denotes the matter-Lagrangian density. Due to the presence of an additional source, the anisotropy in the internal geometry arises. This approach decouples the system by separating the radial metric component. Consequently, the field equations split into two distinct sets, one corresponds to an isotropic source and the other to an anisotropic source. Initially, we substitute the viable non-singular metric solution into the field equations. Afterward, the enlarged system incorporating the additional fluid is solved by applying appropriate boundary conditions to the pressure and density corresponding to both gravitational sources. We investigate the behavior of different cosmic quantities to assess the viability of the compact star. The observed characteristics of physical quantities demonstrate a high-density configuration in the considered stellar candidate. In this gravitational framework, the stability limits are satisfied for both solutions in the presence of decoupling parameter. We conclude that the chosen parametric values provide a stable structure for the solution corresponding to the pressure and density-like constraints.

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