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Black Hole Protects Vacuum from Disturbances ⚡ экспресс

Original: "Dynamical Casimir Effect and Vacuum Friction in the Near-Horizon Geometry of a Black Hole"
arXiv:2605.09783 · 2026-05-10 · CC BY · ⏱ 1 min · General Relativity
At the edge of a black hole, even the sharpest mirror movement won't chip a single particle out of emptiness.
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In empty space, you can chisel out particles just by moving a mirror quickly. But try the same trick at a black hole's horizon—nothing will happen. Gravity demands that oscillations fade in proportion to the distance to the hole, otherwise the mirror would exceed the speed of light. At the very edge, its motion is completely "frozen," leaving the vacuum imperturbable.

🎯 An unexpected twist: the damping of particles isn't due to the quantum nature of the vacuum. It's dictated by pure geometry—to simply not outrun light, the mirror must come to a halt. Quantum laws only slightly tweak this inevitability.

🎬 The scenario recalls scenes from "Interstellar": near a black hole, time freezes, and all rhythms stop—only here it's not fiction but a calculation.

c_{\text{coord}} = c \left(1 - \frac{r_s}{r}\right)
Effective coordinate speed of light near a black hole decreases to zero at the horizon.
Scientists
Christian DopplerD. B. McLaughlinDidier QuelozMichel MayorR. A. RossiterStephen Hawking
Tags
black hole spacetime curvature speed of light
Laws
Doppler effectHawking radiationgravitational lensingprinciple of constancy of the speed of lightBekenstein-Hawking entropymass–energy equivalence
Original: arXiv:2605.09783 · CC BY · bridge42worlds