Abstract
We present a new class of static spherically symmetric exact solutions of the Einstein-Maxwell field equations in isotropic coordinates for perfect fluid by considering a specific choice of electrical intensity which involves a parameter K. The resulting solutions represent charged fluid spheres joining smoothly with the Reissner-Nordstrom metric at the pressure free interface. The solutions so obtained are utilized to construct the models for super-dense star like neutron stars (ρ b =2 and 2.7×1014 g/cm3) and Quark stars (ρ b =4.6888×1014 g/cm3). It is observed that the models are well behaved for the restricted value of parameter K (0.141≤K≤0.159999). Corresponding to K max =0.159999 for which, u max =0.259, the resulting Quark star has a maximum mass M=1.618 M ⊙ and radius R=9.263 km and the neutron star modeling based on the particular solution; corresponding to K=0.15, u=0.238 and by assuming the surface density ρ b =2.7×1014 g/cm3 the maximum mass of neutron star M=1.966 M ⊙ and radius R=12.23 km and by assuming the surface density ρ b =2×1014 g/cm3 the resulting well behaved solution has a maximum mass of neutron M=2.284 M ⊙ and radius R=14.21 km. The robustness of our result is that it matches with the recent discoveries.
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Authors express their sincere gratitude to the reviewer(s) for rigorous review, constructive comments, and useful suggestions. Authors are grateful to Prof. A.N. Srivastava (HOD Mathematics) and Prof. S. Nandi (HOD Physics) for their encouragement and motivation.
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Pradhan, N., Pant, N. Einstein-Maxwell field equations in isotropic coordinates: an application to neutron star and quark star. Astrophys Space Sci 352, 143–149 (2014). https://doi.org/10.1007/s10509-014-1905-z
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DOI: https://doi.org/10.1007/s10509-014-1905-z