variety of well behaved exact solutions of einstein–maxwell field equations: an application to strange quark stars, neutron stars and pulsars

we present a variety of well behaved classes of charge analogues of tolman’s iv (1939). 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 for every positive value of n for which the solution is well behaved hence, suitable for modeling of super dense stars. 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 (0.3 ≤ k ≤ 0.91) for which the solution is well behaved hence, suitable for modeling of super dense stars like strange quark stars, neutron stars and pulsars. for this class of solutions the mass of a star is maximized with all degree of suitability, compatible with quark stars, neutron stars and pulsars. by assuming the surface density ρ_b = 2 × 10¹⁴ g/cm³ (like, brecher and caporaso in nature 259:377, 1976), corresponding to k = 0.30 with x = 0.39, the resulting well behaved model has the mass m = 2.12m_θ, radius r_b ≈ 15.27 km and moment of inertia i = 4.482 × 10⁴⁵ g cm²; for k = 0.4 with x = 0.31, the resulting well behaved model has the mass m = 1.80m_θ, radius r_b ≈ 14.65 km and moment of inertia i = 3.454 × 10⁴⁵ g cm²; and corresponding to k = 0.91 with x = 0.135, the resulting well behaved model has the mass m = 0.83m_θ, radius r_b ≈ 11.84 km and moment of inertia i = 0.991 × 10⁴⁵ g cm². for n = 0 we rediscovered pant et al. (in astrophys. space sci. 333:161, 2011b) well behaved solution. these values of masses and moment of inertia are found to be consistent with other models of neutron stars and pulsars available in the literature and are applicable for the crab and the vela pulsars.