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Stability analysis of dynamic thin shells

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arxiv gr-qc/0507063 v2 pith:7APM74LR submitted 2005-07-14 gr-qc astro-phhep-th

Stability analysis of dynamic thin shells

Francisco S. N. Lobo , Paulo Crawford This is my paper
classification gr-qc astro-phhep-th
keywords analysisstabilityconsideringshellsthinaroundchoicesdeduce
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We analyze the stability of generic spherically symmetric thin shells to linearized perturbations around static solutions. We include the momentum flux term in the conservation identity, deduced from the ''ADM'' constraint and the Lanczos equations. Following the Ishak-Lake analysis, we deduce a master equation which dictates the stable equilibrium configurations. Considering the transparency condition, we study the stability of thin shells around black holes, showing that our analysis is in agreement with previous results. Applying the analysis to traversable wormhole geometries, by considering specific choices for the form function, we deduce stability regions, and find that the latter may be significantly increased by considering appropriate choices for the redshift function.

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Cited by 3 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. Thin-shell wormholes in cosmic voids

    gr-qc 2026-07 unverdicted novelty 5.5

    Symmetric thin-shell wormholes in void-embedded black-hole spacetimes can be stable under a modified cosmic Chaplygin gas but are generically unstable under a generalized cosmic Chaplygin gas.

  2. Thin-shell wormholes in cosmic voids

    gr-qc 2026-07 conditional novelty 5.0

    Thin-shell wormholes can be built inside a cosmic void by gluing two black-hole-in-void spacetimes, and their stability depends sharply on the shell equation of state.

  3. Static Dark Fluid Thin Shells in Schwarzschild-de Sitter Spacetimes: Stability and Black Hole Shadows

    gr-qc 2026-02 conditional novelty 5.0

    Stable static dark-fluid shells separating two Schwarzschild–de Sitter spacetimes exist only for m_+/m_->1 and arise at three scales, imprinting observable black-hole shadow deviations.