Black‑Hole Entropy under GG‑Theory

Abstract

Black holes are the strangest objects in nature. Fifty years ago Stephen Hawking discovered that they are not perfectly black: they glow faintly, and over almost unimaginable spans of time they evaporate away. This discovery created the deepest puzzle in modern physics. Whatever falls into a black hole carries detailed information about what it was; yet the faint glow that leaks back out looks featureless — the same for every black hole of the same size. If the glow truly carries nothing, then that information has been erased, and the erasure of information is something the laws of physics are not supposed to allow. For half a century no one has agreed on how the books are balanced.

This paper offers a resolution built on GG-Theory, a framework in which the world we experience is the surface of a slightly larger six-dimensional space. In that picture the edge of a black hole — its horizon — is not a wall but a doorway: matter that crosses it is not destroyed but carried into directions we cannot see, and the faint glow is simply how that crossing looks from the outside. Nothing is lost; it is only put out of reach. From this single idea, and without adjusting any free number, the paper recovers the famous formula for how much a black hole can hold, explains why the glow should eventually carry the hidden information back out, and shows why the argument that a traveler falling inward must meet a wall of fire does not go through. The same reasoning extends to the horizon of the expanding universe as a whole. The claims are set out so that future telescopes and gravitational-wave detectors can put them to the test.