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

Within semiclassical gravity, Hawking radiation portrays a black hole as a steadily radiating system that ultimately evaporates. Motivated by the gap between unitary “entropy bookkeeping” (for example in holography and the island formula) and concrete 3+1-dimensional dynamical corrections, we introduce a frequency-dependent suppression factor S (ω) in the range [0, 1), induced by cross-horizon entanglement. We parametrize the observable outgoing contribution of the Bogoliubov coefficient β (ω) by defining an effective coefficient βₑff (ω) = (1 − S (ω) ) β (ω), so that occupation numbers and radiated power are uniformly rescaled by (1 − S (ω) ) ². The suppression factor S (ω) can be interpreted as the frequency-space projection of a long-range correlation kernel in the two-point function, and it is required to decay rapidly at high frequencies in order to preserve the standard short-distance (Hadamard) structure. To quantify the impact of this mechanism, we numerically solve the scalar Regge–Wheeler equation in a 3+1-dimensional Schwarzschild background, compute greybody factors for the leading partial waves, and convolve them with a Lorentz-type low-frequency suppression model (for example S₀ = 0. 8 and ωc = 3 TH) to obtain modified spectra and total power. In the scalar minimal setting, the evaporation lifetime is enhanced by a factor Aₛcalar ≈ 2. 30 (more precisely 2. 2988 ± O (10⁻⁴) ), supported by convergence tests and an explicit error budget. Extending the calculation to a multi-spin sum yields a more conservative estimate closer to the total emission, Aₜotal ≈ 1. 94 (with an uncertainty scale of order 10⁻³). For consistency, we also solve the scalar Teukolsky equation in Kerr geometry and scan the superradiant band, finding that the maximal amplification is of order 10⁻³. Combined with the effective dissipation implied by the suppression mechanism, this supports a conservative stability threshold and delineates a safe region in parameter space, indicating dynamical viability in both Schwarzschild and Kerr spacetimes. A minimal consistency check of the generalized second law (GSL) shows that the total entropy production rate can remain non-negative under representative settings and truncations. Observationally, the model predicts systematic low-frequency deviations from the Hawking spectrum and a delayed evaporation and information-release timescale. It permits a first-order rescaling of energy-injection constraints that shifts primordial black hole survival boundaries. If the near-horizon effective structure manifests as a frequency-selective partial reflection in perturbative scattering, the late-time ringdown may exhibit echo-like features with band-selective characteristics. Taken together, these results indicate that within a mildly nonlocal semiclassical effective description, complete black-hole evaporation is not a logical necessity but a conditional process governed by the entanglement structure of the quantum state and the mechanism by which long-range correlations are retrieved.