The stability of thin-shell wormholes with a phantom-like equation of state

TL;DR

This paper analyzes the linear stability of spherically symmetric thin-shell wormholes with a phantom-like equation of state across various black hole spacetimes, extending previous approaches with a new method.

Contribution

It introduces a different analytical approach to stability analysis of thin-shell wormholes with a phantom-like equation of state in diverse black hole backgrounds.

Findings

Stability conditions depend on the specific spacetime geometry.

Certain parameter ranges yield stable wormhole configurations.

The approach generalizes previous stability analyses to more complex spacetimes.

Abstract

This paper discusses the stability to linearized radial perturbations of spherically symmetric thin-shell wormholes with a "phantom-like" equation of state for the exotic matter at the throat: $P=\omega\sigma$, $\omega<0$, where $\sigma$ is the energy-density of the shell and $P$ the surface pressure. This equation is analogous to the generalized Chaplygin-gas equation of state used by E.F. Eiroa. The analysis, which differes from Eiroa's in its basic approach, is carried out for wormholes constructed from the following spacetimes: Schwarzschild, de Sitter and anti de Sitter, Reissner-Nordstrom, and regular charged black-hole spacetimes, as well as from black holes in dilaton and generalized dilaton-axion gravity.