Relativistic modeling of charged super-dense star with Einstein‐Maxwell equations in general relativity

We have obtained a variety of well behaved classes of Charge Analogues of Heintzmann’s solution by using a particular electric intensity, which depends upon two parameter K and n. These solutions describe charged fluid balls with positively finite central pressure, positively finite central density; their ratio is less than one and causality condition is obeyed at the centre. The outmarch of pressure, density, pressure–density ratio and the adiabatic speed of sound is monotonically decreasing, however, the electric intensity is monotonically increasing in nature. These solutions give us wide range of parameter K for every positive value of n for which the solution is well behaved hence, suitable for modeling of super dense stars like neutron stars and pulsars. Keeping in view of well behaved nature of these solutions, one new class of solutions is being studied extensively. Moreover, this class of solutions gives us wide range of constant K (1.3? K ?17.95). Also this class of solutions, the mass of a star is maximized with all degree of suitability, compatible with neutron stars and pulsars. By assuming the surface density ρ b =2×10¹⁴ g/cm³, the whole family of charged solution with well behaved conditions, the maximum mass and corresponding radius is 4.5132M T and 16.9057km respectively.