Advancing the understanding of compact stars: The role of f (R, Lm, T) gravity on physical existence of two different pulsars

Recent studies have demonstrated the possibility of using modified gravity theories in order to explain the sense of astronomical entities. This paper examines the dynamics of dense astronomical entities under the framework of f (R, Lm, T) gravity. We formulate gravitational equations that incorporate the characteristics of the non-isotropic static interior spacetime. By imposing two particular conditions related to the radial function and pressure anisotropy, we derive two solutions to these complex equations of motion. We encounter differential equations in both cases whose solutions involve two constants. The Darmois junction conditions are then employed to calculate these constants. Moreover, the requirement for radial pressure to vanish at the hypersurface is also significant in this analysis. Additionally, we graphically assess specific conditions that must be satisfied to ensure the model's viability across various parameter values. For this purpose, we utilize observational data from two compact stars, Her X-1 and Cen X-3. We conclude that both models align well with the necessary criteria for viability and stability. It is important to emphasize that our study amplifies the understanding of how this modified gravity influences the interior fluid distribution of compact stars, offering invaluable revelations for future studies.