A New Model for Strange Stars

TL;DR

This paper introduces a novel, stable model for strange stars using the Homotopy Perturbation Method to solve Einstein's equations with the MIT bag model EOS, providing a new approach in relativistic astrophysics.

Contribution

First application of the Homotopy Perturbation Method to find singularity-free solutions for strange star models in relativistic astrophysics.

Findings

Model is consistent with Schwarzschild exterior spacetime.

Model satisfies energy conditions and stability criteria.

Predicted parameters match observed strange star candidates.

Abstract

In the present work, we attempt to find a new class of solutions for the spherically symmetric perfect fluid sphere by employing the Homotopy Perturbation Method (HPM), a new tool via which the mass polynomial function facilitates to tackle the Einstein field equations. A set of interior solutions found on the basis of the simplest MIT bag model equation of state (EOS) in the form $p=\frac{1}{3}(\rho-4B)$ where $B$ is the bag constant. The proposed interior metric for the stellar system is consistent with the exterior Schwarzschild spacetime on the boundary. In addition, we also conduct a detailed study on different tests, viz. the energy conditions, TOV equation, adiabatic index, Buchdahl limit, etc., to verify the physical validity of the proposed model. The numerical value of the used parameters is predicted for different strange star candidates, for different chosen values of the bag constant. In a nutshell, by exploiting HPM technique first time ever in the field of relativistic astrophysics, we have predicted in the present literature a singularity-free and stable stellar model which is suitable to describe ultra-dense objects, like strange (quark) stars.