  In this paper, we have constructed a model for well behaved isotropic compact
star in the presence of charged perfect fluid, by considering a static and
spherically symmetric metric in Schwarzschild's canonical coordinate system. To
put the resulting differential equations into a closed system, we have employed
the Vaidya & Tikekar (J. Astrophys. Astron. 3:325, 1982) form of the metric
potential grr. The resulting energy-momentum components, i.e., energy density
and pressure contain six constants; two of these are determined through the
junction condition (matching the interior with the exterior Schwarzschild
solution) and by the property of vanishing pressure on the boundary. The
remaining constants are constrained by requirements of a real compact star. The
physical acceptability of our model is tested using the data of the pulsar PSR
B0943+10. Using graphical analysis and tabular information we have shown that
our model obeys all the physical requirements. The stability of this model is
evaluated using the Tolman-Oppenheimer-Volkoff equation, the adiabatic index
and the Harrison-Zeldovich-Novikov Criterion and it has passed the evaluation.
