Charged Analogues of Isotropic Compact Stars Model with Buchdahl Metric in General Relativity

TL;DR

This paper develops new exact solutions for charged isotropic compact stars using Einstein-Maxwell equations with a specific metric, analyzing their physical stability and compatibility with observed stellar data.

Contribution

It introduces a novel class of solutions for charged isotropic stars in pseudo-spheroidal spacetime, including detailed physical analysis and observational consistency.

Findings

Solutions satisfy physical and energy conditions

Model's physical parameters are monotonically decreasing

Results align with observational data for compact stars

Abstract

In this work, we examine a spherically symmetric compact body with isotropic pressure profile, in this context we obtain a new class of exact solutions of Einstein's-Maxwell field equation for compact stars with uniform charged distributions on the basis of Pseudo-spheroidal space-time with a particular form of electric field intensity and the metric potential g_rr. Indicating these two parameters takes into account further examination to be done in deciding unknown constants and depicts the compact strange star candidates likes PSR J1614-2230, 4U 1608-52, SAX J1808.4-3658, 4U 1538-52, SMC X-1, Her X-1, and Cen X-3. By the isotropic Tolman-Oppenhimer-Volkoff(TOV)equation, We explore the equilibrium among hydrostatic, gravitational and electric forces. Then, we analyze the stability of the model through the adiabatic index(gamma) and velocity of sound (0 <dp/c^2dr< 1). we additionally talk about other physical features of this model like, for example, the pressure, redshift, density, energy conditions and mass-radius of the stars in detail and demonstrate that our results are satisfying all the basic prerequisites of a physically legitimate stellar model. We have seen the measurement of basic physical parameter such as pressure, density, energy and redshift are satisfied the reality condition. All the physical quantities such as density, pressure pressure-density ratio and speed of sound is monotonically decreasing. The outcomes acquired are valuable in exploring the strength of other compact objects like white dwarfs, gravastars and neutron stars. Finally, we have shown that the obtained solutions are compatible with observational data for compact objects.