Decoupled asymmetric thin-shell wormholes
Abstract
We construct reflection-asymmetric thin-shell wormholes by joining a Schwarzschild exterior to its minimal geometric deformation, which shares the same mass and redshift function, so that the asymmetry is carried entirely by the gravitational-decoupling sector. The deformed side is a black hole sourced by a scalar field coupled to nonlinear electrodynamics, in its branch with a real scalar. We show that the total radial null energy of shell and bulk obeys an exact identity and becomes positive for a sufficiently strong deformation. The momentum flux across the shell equals the radial null-energy density of the bulk, and retaining it yields the linear stability condition in closed form. We prove that stability with a conventional shell response requires the bulk to violate the radial null energy condition at the throat; the deformation instead enlarges the stable domain and moves the transition radius inside the photon sphere. For a stationary extension built on Kerr, the junction is solved exactly in the spin, which fixes how the angular momentum is shared between shell and bulk and where the shell behaves as a rotating fluid. A free-precession model provides an estimate of the gravitational-wave signal of the throat.
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BibTeX
@misc{lopezhormazabal2026decoupled,
title = {{Decoupled asymmetric thin-shell wormholes}},
author = {A. López-Hormazábal and Hishan Farfán-Bachiloglu and Kazuharu Bamba and Francisco Tello-Ortiz},
howpublished = {arXiv},
year = {2026},
month = oct,
doi = {10.48550/arxiv.2610.35407},
eprint = {2610.35407},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2610.35407},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Decoupled asymmetric thin-shell wormholes
AU - A. López-Hormazábal
AU - Hishan Farfán-Bachiloglu
AU - Kazuharu Bamba
AU - Francisco Tello-Ortiz
PY - 2026
DA - 2026/10/26
PB - arXiv
DO - 10.48550/arxiv.2610.35407
UR - https://arxiv.org/abs/2610.35407
AB - We construct reflection-asymmetric thin-shell wormholes by joining a Schwarzschild exterior to its minimal geometric deformation, which shares the same mass and redshift function, so that the asymmetry is carried entirely by the gravitational-decoupling sector. The deformed side is a black hole sourced by a scalar field coupled to nonlinear electrodynamics, in its branch with a real scalar. We show that the total radial null energy of shell and bulk obeys an exact identity and becomes positive for a sufficiently strong deformation. The momentum flux across the shell equals the radial null-energy density of the bulk, and retaining it yields the linear stability condition in closed form. We prove that stability with a conventional shell response requires the bulk to violate the radial null energy condition at the throat; the deformation instead enlarges the stable domain and moves the transition radius inside the photon sphere. For a stationary extension built on Kerr, the junction is solved exactly in the spin, which fixes how the angular momentum is shared between shell and bulk and where the shell behaves as a rotating fluid. A free-precession model provides an estimate of the gravitational-wave signal of the throat.
ER -