Finch-Skea dark energy star with anisotropy

Abstract We present relativistic model of anisotropic compact objects with spherically symmetric matter distribution coupled with dark energy in the framework of general theory of relativity. We assumed an ansatz for dark energy (DE) equation of state in addition to the baryonic matter. The interior spacetime of the compact object is described by the Finch-Skea metric and a causal domain of DE with a coupling parameter β. The stellar model is employed to investigate physical features energy-density, radial pressure, transverse pressure, energy conditions, mass-radius relation for a given pulsar, PSR J0348+0432 (M = 2.01 ± 0.04 M⊙ and R = 12.072 km). The effect of DE is explored for different values of β. We test the stability of the stellar models for different values of DE coupling parameter β for a relativistic stellar model. The equation of state of the matter configuration inside the star is determined for different β and found nonlinear. The prescription for a realistic stellar model used for the given pulsar is employed for other pulsars. The equation of states for those pulsars and the model parameters are determined for the observed masses and radii of the pulsars. The EoS is non-linear and the plot of mass vrs. radius of the stellar models considered here predict that the maximum mass of a star is independent of the DE coupling parameter (β).