A theoretical team has built reflection-asymmetric thin-shell wormholes by joining a Schwarzschild exterior to its minimal geometric deformation. Both sides share the same mass and redshift function, so the asymmetry is carried entirely by the gravitational-decoupling sector. The deformed side describes a black hole sourced by a scalar field coupled to nonlinear electrodynamics, in its real-scalar branch.

The work shows that the total radial null energy of shell and bulk obeys an exact identity and becomes positive when the deformation is sufficiently strong. The momentum flux through the shell equals the radial null-energy density of the bulk, and retaining it yields the linear stability condition in closed form. The authors also prove that 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 emitted by the wormhole throat.

The construction offers a framework to study asymmetric wormholes without resorting to exotic matter outside, and opens the door to comparing its predictions — especially the precession signal — with future searches for gravitational lensing and gravitational waves from compact objects.