Tolman VI Fluid Sphere in f(R,T) Gravity

We analyze the behavior of relativistic spherical objects within context modified f(R,T) gravity considering Tolman VI spacetime, where gravitational Lagrangian is a function Ricci scalar (R) and trace energy momentum tensor (T), i.e, = R + 2βT, for some arbitrary constant β. For developing our model, we have chosen £m −p, represents matter Lagrangian. this investigation, three compact stars, namely PSR J1614-2230 (Mass (1.97 ± 0.4)M⊙; Radius 9.69+0.02−0.02 km), Vela X-1 (1.77 0.08)M⊙; 9.560+0.08−0.08 km) 4U 1538-52 (9.69)M⊙; 1.97 km). In theory, equation pressure isotropy identical to standard Einstein’s theory. So, all known metric potential solving equations are also valid here. paper, investigated effort coupling parameter (β) on local distribution. The sound speed adiabatic index higher with grater values β, while contrary, mass redshift lower supporting theoretical results, graphical representations employed physical viability stars.