Integrability of Anisotropic Fluid Configurations of Compact Stellar in Tolman-IV Spacetime in Symmetric Teleparallel Gravity

In this study, we explore compact stellar configurations within the framework of symmetric teleparallel gravity, considering a modified form of the action f(Q), where Q is the non-metricity scalar. Employing the Tolman IV metric potential, we derive exact interior solutions to the field equations and construct physically viable models of compact stars. The junction conditions are applied to smoothly match the interior configuration with the corresponding exterior spacetime in f(Q) gravity. To test the applicability of the model, we analyze three well-known compact stars: 4U 1820-30, PSR J0437-4715, and PSR J1903+327, using their observed masses and radii. The physical viability of the solutions is assessed through a detailed examination of the matter distribution and stability criteria, including the energy density, anisotropic pressures, energy conditions, pressure and density gradients, the generalized Tolman-Oppenheimer-Volkoff equilibrium, sound speed constraints, compactness, mass functions, and adiabatic index. Our results confirm that the obtained configurations are regular, stable, and consistent with the essential features required for realistic stellar objects. The analysis demonstrates that f(Q) gravity, using the Tolman IV metric space, provides a robust theoretical framework for modeling dense stellar structures, yielding predictions that are compatible with observational data and standard requirements for compact stars.