Sparsity of the Hawking flux

Alexander Van-Brunt (Victoria University of Wellington); Finnian Gray (Victoria University of Wellington); Matt Visser (Victoria University of Wellington); Sebastian Schuster (Victoria University of Wellington)

Sparsity of the Hawking flux

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arxiv 1512.05809 v1 pith:64JMTGY7 submitted 2015-12-17 gr-qc hep-th

Matt Visser (Victoria University of Wellington) , Finnian Gray (Victoria University of Wellington) , Sebastian Schuster (Victoria University of Wellington) , Alexander Van-Brunt (Victoria University of Wellington) This is my paper · ORCID

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It is (or should be) well-known that the Hawking flux that reaches spatial infinity is extremely sparse, and extremely thin, with the Hawking quanta, one-by-one, slowly dribbling out of the black hole. The typical time between quanta reaching infinity is much larger than the timescale set by the energy of the quanta. Among other things, this means that the Hawking evaporation of a black hole should be viewed as a sequential cascade of 2-body decays.

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Quantum-Corrected Thermodynamics, Dirac Perturbations, Geodesic Structure, and Topological Phases of Black Holes with Non-Minimal Logarithmic Coupling
gr-qc 2026-07 reject novelty 4.0 of 10

For the ln(R)F² black hole, a single coupling B is claimed to shrink the shadow and ISCO, alter Dirac quasinormal ringing, suppress Hawking luminosity, and set the sign of an effective pressure on the topological defect line.

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