How a Black Hole Digests Information ✎

Original: "Negative entropy in scrambling black holes"
· Koji Azuma
arXiv:2605.25315 · 2026-05-25 · arXiv non-exclusive · independent analysis · 1 min
An object falling into a black hole increases its area by exactly the amount needed to accommodate its energetic footprint.

A black hole is like a perfect safe: anything that goes in seems lost forever. But at the microscopic level, it doesn't destroy information: it shuffles it with its internal degrees of freedom, much like a deck of cards after a thorough shuffle.

The event horizon is not a wall but a one-way membrane: you can't get out, but you can fall in.

In the new work, physicists showed that the area of the horizon (the surface beyond which even light cannot escape) can be viewed as a measure of the quantum information the hole has already absorbed. When an object falls in, its energy increases the area by just the right amount so that the entropy (a measure of disorder) grows according to a universal formula — with a temperature, like a heated body. This is akin to adding hot water to a bath: the temperature barely changes, but the level rises.

A black hole's temperature is inversely proportional to its mass: the heavier the hole, the colder it is.

The most surprising thing: if you compare an infalling particle with outgoing Hawking radiation, their contributions to the information balance cancel out. What remains is only the net influx of energy, and the horizon area changes exactly according to the first law of black hole thermodynamics. So the safe begins to resemble not just a storage unit, but an active information processor.

If a black hole with the mass of the Sun radiated as a perfect black body, its temperature would be only about 60 nanokelvins — billions of times colder than interstellar space.

In Stanisław Lem's novel "Solaris," the ocean-supermind also absorbs information without return, but unlike a black hole, it also responds.

Scientists
Jacob BekensteinStephen HawkingFritz ZwickyKarl SchwarzschildSubrahmanyan ChandrasekharRainer Weiss
Concepts
Bekenstein-Hawking entropy horizon area black hole entropy logarithmic correction Hawking area theorem First law of black hole mechanics Hawking radiation entropic shadow event horizon critical collapse mass inflation third law of thermodynamics enthalpy nuclear reaction mass gap no-hair theorem ringdown innermost stable circular orbit hills mechanism entropic gravity spin parameter