Some analytic models of relativistic compact stars

We present charged anisotropic Durgapal IV interior solutions of the general relativistic field equations in curvature coordinates. These exact solutions can be used to model stable and well-behaved compact stars. Using these solutions we have presented models of well-known neutron and quark stars such as PSR J1903+0327, RX-J1856.5-3754, PSR B1913+16, PSR J0737-3039A and Cyg X-2. The equation of state (EoS) corresponding to the modeled objects are studied using their compression moduli. According to our solutions it is found that the EoS for Cyg X-2 (neutron star) is stiffer than any other object presented and therefore more massive. Furthermore, the EoS for RX J1856.5-3754 (Quark star) is the softest one, rendering it least massive. These solutions satisfy all the energy conditions. Finally, all our presented stellar models satisfy the equilibrium condition of Cooperstock and de la Cruz i.e. M-2 > Q(2).