Charged anisotropic compact stellar models under gravitational decoupling scheme

The aim of this paper is to obtain new physically admissible exact anisotropic stellar models via gravitational decoupling technique. This will be done by taking Korkina and Orlyanskii model solution as a seed solution and extend it to an anisotropic domain via gravitational decoupling through the minimal geometric deformation (MGD) approach. We analyze the physical properties of four compact star models Her X-1 (Mass M = 0.85M Theta, radius=8.1 radius = 8.1 km), LMC X-4 (M = 1.04M Theta, radius = 8.301 radius = 8.301 km), PSR J1903 + 327J1903 + 327 (M = 1.667M Theta, radius = 9. 438 radius = 9.438 km) and PSR J1614-2230J1614 - 2230 (M = 1.97M Theta, radius = 9.69r adius = 9.69 km). We demonstrate the stability conditions of the obtained solution by plotting energy conditions, velocity of sound, adiabatic index and all the thermodynamic parameters and equilibrium conditions via TOV equation, etc. We found that the results are physically well behaved and also fulfill the requirement of stability criteria inside the anisotropic fluid sphere. We study the physical features of the solutions in detail, analytically and graphically for the four compact stars Her X-1, LMC X-4, PSR J1903 + 327J1903 + 327 and PSR J1614 - 2230J1614 - 2230. Based on the results we realized that the extended gravitational decoupling technique is very effective for the analysis of the interior of the compact stellar structures.