Charged Vaidya–Tikekar model for super compact star

In this work, we explore a class of compact charged objects that have been tested against experimental and observational constraints with some known compact stars candidates. This study is performed by considering the self-gravitating, charged, isotropic fluids which are more pliability in solving the Einstein–Maxwell equations. In order to determine the interior geometry, we utilize the Vaidya–Tikekar (J Astrophys Astron 3: 325, 1982) geometry for the metric potential with Riessner–Nordstr o m metric as an exterior solution. These model parameters are determined after selecting some particular values of M and R, for the compact objects SAX J1808. 4-3658, Her X-1 and 4U 1538-52. The most striking consequence is that hydrostatic equilibrium is maintained for different forces, and the situation is clarified by using the generalized Tolman–Oppenheimer–Volkoff equation. In addition to this, we also present the energy conditions, speeds of sound and compactness of stars that are very much compatible to that for a physically acceptable stellar model. Arising solutions are also compared with graphical representations that provide strong evidences for more realistic and viable models, both at theoretical and astrophysical scale.