Tolman VI Fluid Sphere in <i>f</i>(<i>R</i>,<i>T</i>) Gravity

Abstract

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

Keywords

• Tolman VI spacetime
• compact stars
• <i>f(R,T)</i> gravity