Abstract
In the present article, we explore a new static, spherically symmetric charged anisotropic fluid model of compact star in curvature coordinates. We consider metric potential g44 of Durgapal’s fifth solution [1] with a specific choice of electric field intensity E and physically acceptable expression of anisotropy factor Δ , which involve parameters K (charge) and Δ (anisotropy) respectively. The solution so obtained is utilized to construct the model for superdense star like neutron star. We have analysed that corresponding to X=0.1, K=2.8, a=1.6 and by assuming surface density , the mass of the compact star comes out to be with radius 14.51 kms, which closely resembles to that of PSRJ0348 + 0432. The solution is well behaved for the values of K satisfying 1≤K5. Our model is described analytically as well as with the help of graphical representations. Our solution is well behaved and free from any central singularity. It also satisfies all the energy conditions as well as the causality condition thus reconfirming the stability of our model.
Highlights
During the final stages of stellar evolution when the nuclear fuel inside the star is almost exhausted, the star deviates from its hydrostatic equilibrium stage and starts to collapse
Neutron star is composed of neutrons, while strange star is composed of u, d, and s quarks
The formation of strange matter can be categorized in two ways: the quark hadron phase transition in the early universe and conversion of neutron stars into strange stars [2]
Summary
During the final stages of stellar evolution when the nuclear fuel inside the star is almost exhausted, the star deviates from its hydrostatic equilibrium stage and starts to collapse. Fuloria providing stability to it against gravitational collapse Compact objects such as white dwarf stars, neutron stars, strange stars and black holes represent the final stages of a star’s evolution. The study of relativistic models of compact stars like neutron stars and strange stars have been a field of active research in recent years. It is interesting to note that by relaxing the condition of a perfect fluid and allowing for pressure anisotropy and charge within the interior of stellar configurations, more realistic structure of compact stellar objects can be realized. Compact stellar models for neutral/charged static spherically symmetric configuration with anisotropic pressure have been obtained in numerous works. We assume some particular forms of electric charge distribution function and pressure anisotropy so that we may construct a physically reasonable models of stellar objects. In the last section we conclude all results obtained after complete analysis of newly obtained solution
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