Charged gravastars in Rastall-Rainbow gravity

Abstract

In this work, we have assumed the spherically symmetric stellar system in the contexts of Rastall-Rainbow gravity theory in the presence of isotropic fluid source with electro-magnetic field. Einstein-Maxwell’s field equations have been written in the framework of Rastall-Rainbow gravity. Next, we have discussed the geometry of charged gravastar model. The gravastar consists of three regions: interior region, thin shell region, and exterior region. In the interior region, the gravastar follows the equation of state (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 calculated. Finally, we have explored the stability of the charged gravastar in Rastall-Rainbow gravity.