Abstract
In this work, a physically reasonable metric potential $$g_{rr}$$grr and a specific choice of the anisotropy has been utilized to obtain closed-form solutions of the Einstein field equation for a spherically symmetric anisotropic matter distribution. This class of solution has been used to develop viable models for observed pulsars. Smooth matching of interior spacetime metric with the exterior Schwarzschild metric and utilizing the condition that radial pressure is zero across the boundary leads us to determine the model parameters. A particular pulsar $$4U1820-30$$4U1820-30 having current estimated mass and radius ($$mass=1.58 M_\odot $$mass=1.58M⊙ and $$radius=9.1$$radius=9.1 km) has been allowed for testing the physical acceptability of the developed model. The gross physical nature of the observed pulsar has been analyzed graphically. The stability of the model is also discussed given causality conditions, adiabatic index and generalized Tolman–Oppenheimer–Volkov (TOV) equation under the forces acting on the system. To show that this model is compatible with observational data, few more pulsars have been considered, and all the requirements of a realistic star are highlighted. Additionally, the mass-radius (M–R) relationship of compact stellar objects analyzed for this model. The maximum mass for the presented model is $$\approx 4M_\odot $$≈4M⊙ which is compared with the realization of Rhoades and Ruffini (Phys Rev Lett 32:324, 1974).
Modified Finch and Skea stellar model compatible with observational data
