What lurks at the core of an evaporating black hole? ✛ ✎ ✦

Original: "A Quantum Singularity Theorem for the Evaporating Black Hole"
· Netta Engelhardt, Ivri Nagar
arXiv:2605.05326v1 · 2026-05-06 · arXiv non-exclusive · independent analysis · 1 min
Scientists have rigorously proved: as a black hole evaporates, an irreparable tear stays at its center: it doesn’t heal until the last drop.

A black hole works like a whirlpool in a pond: everything falls in and gets squeezed into a point where spacetime tears. That’s the singularity. Water in the pond evaporates, the whirlpool shallows, but the hole at the bottom stays until the very last drop. So it is with a black hole: quantum fields make it dwindle (this was discovered by Stephen Hawking in 1974), yet the singularity never goes away.

The paradox: the very fields that steal the hole’s energy inevitably create the tear. Without them, the singularity wouldn’t have formed in the first place. This insight is crucial for the mystery of information: if the tear never heals, swallowed data likely isn’t erased but gets stuck there. Some theorists link this to wormholes, bridges to other worlds, while a complete answer is sought through string theory.

Physicist Jacob Bekenstein introduced the concept of black hole entropy (a measure of disorder), tying it to the horizon’s area. It was a revolutionary idea that still excites theorists today.

In the movie 'Interstellar', the black hole’s singularity serves as a data channel — a fantasy about how quantum entanglement could link entire universes.

S_{\text{gen}} = \frac{\text{Area}}{4G} + S_{\text{vN}}
S_gen — generalized entropy, Area — horizon area, G — Newton's gravitational constant, S_vN — von Neumann entropy of quantum fields.
Scientists
Roger PenroseStephen HawkingJacob BekensteinFritz ZwickyKarl SchwarzschildSubrahmanyan Chandrasekhar
Concepts
black hole singularity non singular black hole naked singularity modified gravity singularities no-hair theorem remnant semiclassical gravity quantum bounce quantum corrections Hawking area theorem hawking radiation mechanism information loss gravitational atom gravastar complementarity principle null energy condition event horizon stability non singular cosmology Kepler's second law superfluidity