Charged Vaidya-Tikekar model for super compact star

TL;DR

This paper develops a charged Vaidya-Tikekar model for super compact stars, demonstrating its consistency with observational data and physical conditions, and analyzing stability and structure through Einstein-Maxwell equations.

Contribution

It introduces a new charged star model using Vaidya-Tikekar geometry, tested against observational constraints and analyzed with TOV equations for stability.

Findings

Hydrostatic equilibrium maintained for various forces.

Energy conditions and sound speeds are physically acceptable.

Model fits observational data for specific compact stars.

Abstract

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.