An Interior model of Charged Fluid Spheres

At constant time $t$, we examine the Vaidya-Tikekar metric characterising a three-dimensional, extremely dense spheroidal star configuration. The static, spherically symmetric solution of Einstein's field equations can be expressed in analytic closed form utilising a hypergeometric series. A relativistic, superdense state of matter at a constant $t$ is represented by the resultant model, which describes the geometry of a three-spheroid. Assuming a stellar density of $\rho_{a}= 2*10^{14} gm*cm^{-3}$, we investigate configurations whose total mass and radius vary over a range of well-defined values of the density variation parameter. Similar to an uncharged neutron star, all models possess the same total mass and boundary radius. The hypergeometric solution leads to a new class of exact, physically acceptable solutions. We show that the model satisfies the conditions of hydrostatic equilibrium and fulfils all standard energy conditions, which are verified throughout the analysis.