Self bound compact stars in f ( R, T) gravity admitting CFL equation of state in presence of non-minimal QCD correction factor

The present article illustrates a method of generating exact solution for a class of isotropic compact objects in the context of f ( R, T) theory of gravity based on a linear form of the function f ( R, T) as f ( R, T) = R + 2 /3T . The internal matter is assumed to be de-confined quarks described by a colour flavour locked (CFL) equation of state. To obtain exact solution of the field equations, a specific ansatz has been assumed for the g rr metric component as proposed by Vaidya and Tikekar. This type of metric ansatz generally describes the interior space-time geometry of a compact object to be 3-spheroid in nature which is embedded in a four dimensional Euclidean flat space. The equation of state in CFL phase has been modified by introducing a QCD correction term cc or which has significant effects on the equation of state and energy per baryon of quark matter. The f(R,T) theory and CFL phase equation state permit our model to adopt a wider class of compact objects such as EXO 1745-248, LMC X-4, PSR J0740+6620 etc. The observed radii of these compact objects agree with those obtained from our model. The radius of the recently detected binary neutron star merger event GW 230529-181500 having mass 3.6 M ae can also be predicted from our model.