Quantum width of spherically symmetric black hole horizons is defined by signal escape timing and calculated in perturbative quantum gravity to often greatly exceed the Planck length, scaling as sqrt(l_P r_s^2 / sigma_perp) for Schwarzschild patches.
From Asymptotically Flat Gravity to Finite Causal Diamonds
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abstract
We demonstrate that the phase space of the soft sector of asymptotically flat gravity in four spacetime dimensions can be identified with that of a spherically symmetric finite casual diamond in Minkowski spacetime. The leading soft graviton mode is geometrically identified with the radial fluctuation of the causal diamond size, while the Goldstone mode involves both the radial fluctuation and its symplectic partner. This allows us to relate the radial fluctuations of the causal diamond with the asymptotic transverse fluctuations parametrized by the soft modes.
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hep-th 2years
2026 2verdicts
UNVERDICTED 2representative citing papers
Phase space of arbitrary null cut in Minkowski spacetime is symplectomorphic to infrared phase space of asymptotically flat gravity, mapping cut fluctuations to leading soft graviton mode and supertranslation Goldstone mode to cut size times null time offset.
citing papers explorer
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Quantum Fluctuations of the Black Hole Horizon
Quantum width of spherically symmetric black hole horizons is defined by signal escape timing and calculated in perturbative quantum gravity to often greatly exceed the Planck length, scaling as sqrt(l_P r_s^2 / sigma_perp) for Schwarzschild patches.
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Mapping the Infrared Phase Space of Gravity to Finite Subregions
Phase space of arbitrary null cut in Minkowski spacetime is symplectomorphic to infrared phase space of asymptotically flat gravity, mapping cut fluctuations to leading soft graviton mode and supertranslation Goldstone mode to cut size times null time offset.