Relativistic Krori‐Barua Compact Stars in f(R,T)$f(R,T)$ Gravity

This work aims to investigate the behaviour of compact stars in the background of f(R,T)$f(R, T)$ theory of gravity. For current work, we consider the Krori‐Barua metric potential i.e., ν(r)=Br2+C$\nu (r)= Br^2+C$ and λ(r)=Ar2$\lambda (r)= Ar^2$ , where, A,B$A, B$ and C are constants. We use matching conditions of spherically symmetric space‐time with Schwarzschild solution as an exterior geometry and examine the physical behaviour of stellar structure by assuming the exponential type f(R,T)$f(R, T)$ gravity model. In the present analysis, we discuss the graphical behaviour of energy density, radial pressure, tangential pressure, equation of state parameters, anisotropy and stability analysis respectively. Furthermore, an equilibrium condition can be visualized through the modified Tolman‐Oppenheimer‐Volkov equation. Some extra features of compact stars i.e. mass‐radius function, compactness factor and surface redshift have also been investigated. Conclusively, all the results in current study validate the existence of compact stars under exponential f(R,T)$f(R, T)$ gravity model.