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Abstract:We present a deliberately speculative model for the late evolution of a rotating (Kerr) black hole in which a long‑lived reservoir of weakly interacting fermions—taken here to be neutrinos—persists inside the horizon and is supported, in part, by degeneracy pressure. Degeneracy pressure is a standard, temperature‑independent consequence of Fermi–Dirac statistics and underlies the stability of white dwarfs and neutron stars. Building on this well‑established microphysics, we ask a “what if” question: if a degenerate neutrino population could remain in a compact configuration within a non‑singular or effectively reflecting interior, then continued Hawking evaporation would shrink the horizon and could eventually remove the geometric confinement of the fermion reservoir. We derive a parametric release condition by comparing the Kerr horizon scale with the characteristic radius of a self‑gravitating degenerate fermion configuration and show how black hole spin shifts the threshold through the horizon radius. The resulting event would be electromagnetically dark (neutrino‑dominated) but could produce a transient gravitational signature due to rapid mass–energy redistribution. We emphasize that the existence and long‑term persistence of a trapped neutrino reservoir inside an astrophysical black hole is not established by classical general relativity; this work is intended as a phenomenological thought experiment that connects familiar degenerate fermion physics to open questions about black hole interiors and end states.