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PreprintCC BY 4.0arXiv

Exact radial stability threshold for a Minkowski-Schwarzschild thin shell

  • Anuar Idrissov
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Abstract

We study the stability of a thin shell of ordinary matter that separates a flat interior from a Schwarzschild exterior, which is the simplest model of a subluminal warp drive. The matter content of the shell is fixed by the junction conditions and satisfies all the standard energy conditions except very close to the horizon. For a shell made of causal matter we find an exact radius below which it cannot be stable under radial perturbations. We then place a black hole inside the shell and show that this radius grows with the black hole mass, so that the flat interior is the most favourable case. Since such shells are known to be unstable to non-radial perturbations, our result marks the boundary of the region in which any stabilising mechanism would have to operate.

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Cite

BibTeXRIS
BibTeX
@misc{idrissov2026exact,
  title = {{Exact radial stability threshold for a Minkowski-Schwarzschild thin shell}},
  author = {Anuar Idrissov},
  howpublished = {arXiv},
  year = {2026},
  month = oct,
  doi = {10.48550/arxiv.2610.17629},
  eprint = {2610.17629},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2610.17629},
  note = {CC BY 4.0},
}
RIS
TY  - UNPB
TI  - Exact radial stability threshold for a Minkowski-Schwarzschild thin shell
AU  - Anuar Idrissov
PY  - 2026
DA  - 2026/10/13
PB  - arXiv
DO  - 10.48550/arxiv.2610.17629
UR  - https://arxiv.org/abs/2610.17629
AB  - We study the stability of a thin shell of ordinary matter that separates a flat interior from a Schwarzschild exterior, which is the simplest model of a subluminal warp drive. The matter content of the shell is fixed by the junction conditions and satisfies all the standard energy conditions except very close to the horizon. For a shell made of causal matter we find an exact radius below which it cannot be stable under radial perturbations. We then place a black hole inside the shell and show that this radius grows with the black hole mass, so that the flat interior is the most favourable case. Since such shells are known to be unstable to non-radial perturbations, our result marks the boundary of the region in which any stabilising mechanism would have to operate.
ER  -