The Non-Inevitability of Black Hole Evaporation: A Nonlocal Annihilation Model Based on Cross-Horizon Quantum Entanglement

Within the semiclassical gravity framework, Hawking radiation depicts a black hole as an object that steadily emits energy and ultimately evaporates. When combined with the requirement of unitarity, however, this picture raises the question of how the radiation flux, occupation numbers, and two-point functions should be modified at the dynamical level. Motivated by this issue, we introduce a frequency-dependent suppression factor , induced by cross-horizon entanglement, and modify the outgoing Bogoliubov coefficients as , so that the emitted occupation numbers and total power are uniformly rescaled by . The factor can be interpreted as the frequency-space projection of a long-range correlation kernel in the two-point function, and its rapid decay at high frequencies ensures consistency with the standard short-distance structure. To assess the quantitative impact of this mechanism, we solve the scalar Regge–Wheeler equation in a 3+1-dimensional Schwarzschild background and compute greybody factors for the dominant partial waves . Convolving these with a physically motivated low-frequency suppression model yields modified spectra and total power. For representative parameters, we find that the evaporation lifetime is extended to . We further solve the scalar Teukolsky equation in Kerr geometry and compute the superradiant reflection coefficient, finding that the amplification is only , while the effective dissipation introduced by in the relevant frequency band is significantly larger, naturally quenching potential black-hole-bomb instabilities. The model is therefore dynamically stable in both Schwarzschild and Kerr spacetimes. On the observational side, the effective near-horizon structure implied by , together with the angular-momentum barrier, forms a resonant cavity that produces gravitational-wave echoes with a low-pass filtering character during the ringdown stage of binary black-hole mergers. Moreover, the modified evaporation power and lifetime shift the mass window in which primordial black holes can survive, allowing certain mass ranges that would have evaporated in the standard scenario to remain long-lived, thereby opening new parameter space for dark-matter candidates in the band. Taken together, the numerical and theoretical results indicate that complete black-hole evaporation is not a logical necessity of semiclassical gravity, but rather a conditional process governed by the entanglement structure of quantum states and the mechanism by which long-range correlations are recovered.