  In this work, we explore a class of compact charged spheres that have been
tested against experimental and observational constraints with some known
compact stars candidates. The study is performed by considering the
self-gravitating, charged, isotropic fluids which is more pliability in solving
the Einstein-Maxwell equations. In order to determine the interior geometry, we
utilize the Vaidya-Tikekar geometry for the metric potential with
Riessner-Nordstrom metric as an exterior solution. In this models, we determine
constants 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
(TOV) 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.
