A New Model for Strange Stars

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.

arXiv comment19 pages, 8 figures, 2 tables, major revision

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• Anisotropic compact stars in the mimetic gravitational theory
• Interior solutions of relativistic stars in the scale-dependent scenario
• Interior solutions of relativistic stars with anisotropic matter in scale-dependent gravity
• Anisotropic stars made of exotic matter within the complexity factor formalism
• Radial oscillations and tidal Love numbers of dark energy stars
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• Linear and Riccati equations in generating functions for stellar models in general relativity
• Anisotropic Dark Matter Stars
• Model of hybrid star with baryonic and strange quark matter in Tolman-Kuchowicz spacetime
• Tidal deformability and radial oscillations of anisotropic polytropic spheres
• Quark stars with isotropic matter in Hořava gravity and Einstein-æther theory
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