Charged Gravastars in Rastall-Rainbow Gravity

TL;DR

This paper investigates charged gravastars within Rastall-Rainbow gravity, deriving solutions for different regions, analyzing physical properties, and exploring stability, highlighting the influence of Rastall and Rainbow parameters.

Contribution

It provides new analytical solutions for charged gravastars in Rastall-Rainbow gravity, including interior, shell, and exterior regions, and examines their physical properties and stability.

Findings

Physical quantities depend on Rastall and Rainbow parameters.

Analytical solutions for thin shell and interior regions are derived.

Stable regions of charged gravastars are identified.

Abstract

In this work, we have considered the spherically symmetric stellar system in the contexts of Rastall-Rainbow gravity theory in presence of isotropic fluid source with electromagnetic field. The Einstein-Maxwell's field equations have been written in the framework of Rastall-Rainbow gravity. The gravastar consists of three regions: interior region, thin shell region and exterior region. In the interior region, the gravastar follows the equation of sate (EoS) $p=-\rho$ and we have found the solutions of all physical quantities like energy density, pressure, electric field, charge density, gravitational mass and metric coefficients. In the exterior region, we have obtained the exterior Riessner-Nordstrom solution for vacuum model ($p=\rho=0$). Since in the shell region, the fluid source follows the EoS $p=\rho$ (ultra-stiff fluid) and the thickness of the shell of the gravastar is infinitesimal, so by the approximation $h~(\equiv A^{-1})\ll 1$, we have found the analytical solutions within the thin shell. The physical quantities like the proper length of the thin shell, entropy and energy content inside the thin shell of the charged gravastar have been computed and we have shown that they are directly proportional to the proper thickness of the shell ($\epsilon$) due to the approximation ($\epsilon\ll 1$). The physical parameters significantly depend on the Rastall parameter and Rainbow function. Next we have studied the matching between the surfaces of interior and exterior regions of the charged gravastar and using the matching conditions, the surface energy density and the surface pressure have been obtained. Also the equation of state parameter on the surface, mass of the thin shell, mass of the gravastar have been obtained. Finally, we have explored the stable regions of the charged gravastar in Rastall-Rainbow gravity.