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 $f(R,T)=R+2\beta T$. 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 $c_{cor}$ 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 $M_{\odot }$ can also be predicted from our model.