Abstract
We obtain a new class of charged super-dense star models after prescribing particular Forms of the metric potential and electric intensity. The metric describing the superdense stars joins smoothly with the Reissner-Nordstrom metric at the pressure free boundary. The interior of the stars possess their energy density, pressure, pressure density ratio and velocity of sound to be monotonically decreasing towards the pressure free interface. In view of the surface density ρb=2×1014g/cm3, the heaviest star occupies a mass 5.523 M⊙with its radius 13.98 km. In absence of the charge we are left behind with the regular and well behaved fifth model of Durgapal [1].
Highlights
Exact interior solutions of the Einstein-Maxwell field equations joining smoothly to the Nordstrom solution at the pressure free interface are gathering big applause due to some of the following reasons: 1) Gravitational collapse of a charged fluid sphere to a point singularity may be avoided. 2) Solutions of Einstein-Maxwell equations are useful in the study of cosmic sensership. 3) Chargeddust models and electromagnetic mass models are expected to provide some clue about structure of an electron
On account of the nonlinearity of Einstein-Maxwell field equations, not many realistic well behaved, analytic solutions are known for the description of relativistic charge fluid spheres
These coupled solutions are well behaved with some positive values of charge parameter K and completely describe interior of the super-dense astrophysical object with charge matter
Summary
Exact interior solutions of the Einstein-Maxwell field equations joining smoothly to the Nordstrom solution at the pressure free interface are gathering big applause due to some of the following reasons: 1) Gravitational collapse of a charged fluid sphere to a point singularity may be avoided. 2) Solutions of Einstein-Maxwell equations are useful in the study of cosmic sensership. 3) Chargeddust models and electromagnetic mass models are expected to provide some clue about structure of an electron. For well behaved model of relativistic star with charged and perfect fluid matter, following conditions should be satisfied (Pant et al [2]): 1) The solution should be free from physical and geometrical singularities i.e. finite and positive values of central pressure, central density and non zero positive values of e and e . These coupled solutions are well behaved with some positive values of charge parameter K and completely describe interior of the super-dense astrophysical object with charge matter. In the present paper we have obtained yet another new parametric class of well behaved exact solutions of Einstein-Maxwell field equations, which is compatible within the range of Neutron star and quark star
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