Stabilizing Spherical Energy Shells with Angular Momentum in Gravitational Backgrounds

TL;DR

This paper investigates how slow rotation can stabilize spherical energy shells in gravitational backgrounds, potentially mimicking black holes without singularities by balancing gravitational effects through angular momentum.

Contribution

It introduces a model for rotating fluid shells using Israel junction conditions, demonstrating stabilization effects analogous to deSitter gravity in gravastars.

Findings

Angular velocity stabilizes shell radius evolution.

Rotating shells can imitate black holes without singularities.

Stability depends on background spacetime parameters.

Abstract

Spherical energy shells in General Relativity tend to collapse due to gravitational effects and/or due to tension effects. Shell stabilization may be achieved by modifying the gravitational properties of the background spacetime. Thus, gravastars consist of stiff matter shells with an interior deSitter space and an exterior Schwarzshild spacetime whose attractive gravity balances the interior repulsive gravity of the interior deSitter spacetime leading to a stable stiff matter shell. Similar stabilization effects may be achieved by considering rotating shells. Here we study the stability of slowly rotating fluid shells. We show that the angular velocity of the shell has stabilizing properties analogous to the repulsive deSitter gravity of the interior of a gravastar. We thus use the Israel junction conditions and the fluid equation of state of the rotating shell to construct the dynamical equations that determine the evolution of the rotating shell radius. These dynamical equations depend on the parameters of the background spacetime and on the angular velocity of the shell. Assuming a rotating interior and a Schwarzschild exterior spacetime we show that the angular velocity of the shell has interesting stabilizing properties on the evolution of its radius R. Thus rotating matter (or vacuum) shells can imitate black holes while avoiding the presence of a singularity and without the presence of an interior deSitter space.