Abstract
In this present work, we have obtained a singularity-free spherically symmetric stellar model with anisotropic pressure in the background of Einstein’s general theory of relativity. The Einstein’s field equations have been solved by exploiting Tolman ansatz [Richard C Tolman, Phys. Rev. 55:364, 1939] in (3+1)-dimensional space-time. Using observed values of mass and radius of the compact star PSR J1903+327, we have calculated the numerical values of all the constants from the boundary conditions. All the physical characteristics of the proposed model have been discussed both analytically and graphically. The new exact solution satisfies all the physical criteria for a realistic compact star. The matter variables are regular and well behaved throughout the stellar structure. Constraints on model parameters have been obtained. All the energy conditions are verified with the help of graphical representation. The stability condition of the present model has been described through different testings.
Highlights
When densities of compact stars are greater than the nuclear matter density, it expects the appearance of unequal principal stresses, called anisotropic effect
We have presented a model of Einstein’s field equations for a spherically symmetric stellar object with anisotropic pressures
For this particular motive we have selected the Tolman-spacetime as interior geometry, and it has been traditionally matched with the Exterior Schwarzschild geometry to evaluate unknown parameters present in the model
Summary
When densities of compact stars are greater than the nuclear matter density, it expects the appearance of unequal principal stresses, called anisotropic effect. Zubair and Abbas [24] explored charged anisotropic compact stars in f (T ) gravity based on the diagonal form of tetrad field for static spacetime. Biswas and his collaborators [25] used metric potentials given by Krori–Barua [26] and established a new model for highly compact anisotropic strange system in the context of f (R, T ) gravity. In this study we use the Tolman spacetime [45] as spherically symmetry to explore the anisotropy of the heavenly objects named as compact stars. We have investigated the physical stability and viability of anisotropic model of compact stars in the background of the Tolman spacetime.
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