A Non-Singular Evolutionary Model for Black Hole to White Hole Horizon Transitions and Dark Matter Production Abstract: Standard cosmological frameworks modeling black hole interiors via classical general relativity inevitably result in physical singularities, where mathematical density limits break down. This paper introduces a alternative evolutionary model that resolves the singularity boundary problem while simultaneously addressing the black hole information paradox. We postulate that the core of a collapsed stellar or galactic mass does not form an infinitely dense point, but rather stabilizes as a non-singular, high-density "storage sphere" that structurally preserves infalling quantum information. Under this framework, the core acts as an electromagnetically isolated reservoir coupled to the dark sector. As a dying black hole evaporates to a critical Planckian threshold, it undergoes a localized quantum bounce rather than complete dissipation. This mechanism drives a rapid metric inversion of the event horizon into a short-lived white hole horizon, releasing trapped energy over a millisecond timescale. We explore the observational signatures of this transition, analyzing how these high-energy isotropic fluxes can be isolated from standard astrophysical backgrounds in existing transient datasets (e.g., Gamma-Ray Bursts and Fast Radio Bursts). This framework provides a unified model linking end-state horizon mechanics to potential production vectors for galactic dark matter without requiring unstable, prolonged Einstein-Rosen bridges.

Amey Buchake · Zenodo (CERN European Organization for Nuclear Research) (2026)