Anisotropic compact stars in f(R) gravity

We derive a new interior solution for stellar compact objects in $f\mathcal{(R)}$ gravity assuming differential relation to constrain the Ricci curvature scalar. To this aim, we consider specific forms radial component of metric and first derivative $f\mathcal{(R)}$. After, time potential form $f(\mathcal R)$ function are derived. From these results, it is possible obtain tangential components pressure density. The resulting represents physically motivated anisotropic neutron star model. It match with boundary exterior solution. matching, potentials can be rewritten terms compactness parameter $C$ which has $C=2GM/Rc^2 <<0.5$ physical consistency. Other conditions real taken into account according show that model accurately bypasses like finiteness pressures, energy density at center star, positivity through structure, negativity gradients. These satisfied if energy-conditions hold. Moreover, study stability by showing Tolman-Oppenheimer-Volkoff equation hydrostatic equilibrium. matched observational data millisecond pulsars withe dwarf companion presenting thermonuclear bursts.