Finch-Skea dark energy star with anisotropy

We present a 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 the dark energy (DE) equation of state (EoS) in addition to the baryonic matter. The interior spacetime of the compact object is described by the Finch-Skea (FS) metric and a causal domain of DE with a coupling parameter \(\beta \). The stellar model is employed to investigate physical features such as energy density, radial pressure, transverse pressure, anisotropy, mass-radius relation, EoS, etc. for a known pulsar, PSR J0348+0432 (\(M = 2.01 \pm 0.04 M_{\odot }\) and \(R = 12.072\) km) taking different \(\beta \). We test the stability of the stellar models for various values of \(\beta \) in a relativistic stellar model. The EoS of the matter configuration inside the star is determined for different \(\beta \) which are non-linear. The EoS obtained varying the DE coupling parameter (\(\beta \)) indicates that the matter inside the DE star is more stiff for less \(\beta \). The prescription for obtaining a realistic stellar model is used to employ for other pulsars. The equation of states for those pulsars and the model parameters are determined for their observed masses and radii. The Mass-Radius (M-R) relation is independent of the coupling parameter \(\beta \) and the M-R relation is consistent with the observational constraints.