Sabu M. C | Searcharxiv

arXiv2026

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 $ρ_{a}= 2*10^{14} gm*cm^{-3}$, 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.

gr-qc↗

arXiv2026

A Precise Ultra - Dense Star Model on Spheroidal Space-Time

This study presents a static, spherically symmetric configuration in which the interior geometry of a relativistic superdense star is modeled as a three-spheroid with constant $t_1$. The model is constructed using an analytical closed-form solution to Einstein's field equations. Assuming a characteristic density of $ρ_{a}= 2\times10^{14} \mathrm{g\,cm^{-3}}$, we compute the total mass and radius of the star based on a prescribed set of structural parameters that influence the density profile. The resulting stellar configurations exhibit boundary radii and total masses comparable to those of neutron stars with vanishing charge density. New exact solutions are obtained by solving the relevant second-order ordinary differential equations. We demonstrate that these solutions satisfy the standard energy conditions and maintain hydrostatic equilibrium throughout the stellar interior. All physical requirements remain valid at every point within the configuration. In this framework, the parameter $λ=\frac{ρ_{a}}{ρ_{0}}$ serves as a key determinant of the mass-radius relationship. We further assess the suitability of the model for representing a relativistic superdense star and analyze its stability under radial perturbations. The investigation indicates that, for the configuration to remain dynamically stable, the density ratio between the outer and inner regions must take the value $λ= 0.4$.

gr-qc↗