The Horizon Breathes: How Black Hole Walls Move ✎ express

Original: "A Constraint-Free Formulation of Black Hole Thermodynamics from the Field Equations"
arXiv:2605.08235 · 2026-05-07 · arXiv non-exclusive · independent analysis · 2 min
To understand black hole heat, physicists had to let both horizons wiggle, not just the outer one.

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A black hole is not a frozen sphere. It's more like a soap bubble, whose walls can expand and contract. It even has two layers: the outer horizon, beyond which light cannot return, and the inner one, hidden deeper. When the hole swallows matter or loses energy, both layers shift, like the film of a bubble changing size.

Previously, when deriving the energy conservation law for a black hole (the analogue of the first law of thermodynamics), physicists artificially fixed the inner horizon. They multiplied Einstein's equations by the change in volume, but only for the outer boundary. This worked, but it was like trying to describe breathing while holding one nostril shut. The new approach lets both horizons move simultaneously. Instead of volume change, it uses the change in entropy — a measure of disorder, which for a black hole is tied to the horizon area. The field equations, written on each horizon, are multiplied by the corresponding entropy change, and everything combines into a single law without extra props.

Black hole entropy is enormous: for a hole with the mass of the Sun, it is a billion trillion times larger than that of the Sun itself. This means a black hole is the most capacious store of information in nature.

The method turned out to be surprisingly robust. It works not only in Einsteinian gravity but also in theories with higher derivatives — more complex versions where spacetime curves in trickier ways. The authors also showed that for holes with three independent characteristics (mass, spin, charge), old schemes relying only on horizon radii break down. The correct path is to consider changes directly in the space of these three parameters, like coordinates on a map. Then the first law of thermodynamics emerges naturally, without additional constraints.

If the inner horizon were truly frozen, the hole couldn't evolve smoothly. It's like trying to turn the steering wheel without moving the wheels — formally possible, but physically meaningless.

The area of a black hole's horizon never decreases: this is akin to the law of entropy non-decrease in ordinary physics. Stephen Hawking showed that holes can still lose mass through quantum radiation, but then entropy is carried away by the radiation, and the overall balance is maintained.

In Dan Simmons' novel 'Hyperion', the Time Tombs are surrounded by anti-entropic fields that move backward along the thermal arrow, like the inner horizon of a hole, living by its own rules.

Scientists
Stephen HawkingJacob BekensteinRoger PenroseFritz ZwickyKarl SchwarzschildSubrahmanyan Chandrasekhar
Concepts
First law of black hole mechanics hawking area law black hole thermodynamics wald entropy schwarzschild metric horizon area kerr metric Einstein field equations barrow entropy general relativity modified gravity theories logarithmic correction no-hair theorem entropic shadow tidal charge newtonian limit first principles calculations modified gravity singularities Friedmann equations quantum field theory in curved spacetime