Einstein-Maxwell field equations in isotropic coordinates: an application to neutron star and quark star

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 (rho (b) =2 and 2.7x10(14) g/cm(3)) and Quark stars (rho (b) =4.6888x10(14) g/cm(3)). It is observed that the models are well behaved for the restricted value of parameter K (0.141a parts per thousand currency signKa parts per thousand currency sign0.159999). Corresponding to K (max) =0.159999 for which, u (max) =0.259, the resulting Quark star has a maximum mass M=1.618 M (aS (TM)) 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 rho (b) =2.7x10(14) g/cm(3) the maximum mass of neutron star M=1.966 M (aS (TM)) and radius R=12.23 km and by assuming the surface density rho (b) =2x10(14) g/cm(3) the resulting well behaved solution has a maximum mass of neutron M=2.284 M (aS (TM)) and radius R=14.21 km. The robustness of our result is that it matches with the recent discoveries.