2020/04/10 by Pei-Ming Ho, Ho, Pei-Ming, Yuki Yokokura +1 · 6 citations
Mathematics · Physics and Astronomy · #Black Holes and Theoretical Physics #Black hole (networking) #Charged black hole #Classical mechanics #Cosmology and Gravitation Theories #Curvature #Effective field theory #Einstein #FOS: Physical sciences #False vacuum #Firewall (physics) #General Relativity and Quantum Cosmology (gr-qc) #Geometry #Gravitation #High Energy Physics - Theory (hep-th) #Horizon #Mathematical physics #Mathematics #Minkowski space #Physics #Quantum Electrodynamics and Casimir Effect #Quantum mechanics #Schwarzschild radius #Theoretical physics #Unruh effect #gr-qc #hep-th
paper · pdf · doi:10.48550/arxiv.2004.04956
published in arXiv (Cornell University) (Cornell University) · 37 pages, 2 figures
openalex publication_date 2020/04/10 · arxiv created 2020/11/01 · arxiv updated 2020/11/03 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/08
For an effective field theory in the background of an evaporating black hole with spherical symmetry, we consider non-renormalizable interactions and their relevance to physical effects. The background geometry is determined by the semi-classical Einstein equation for an uneventful horizon where the vacuum energy-momentum tensor is small for freely falling observers. Surprisingly, after Hawking radiation appears, the transition amplitude from the Unruh vacuum to certain multi-particle states grows exponentially with time for a class of higher-derivative operators after the collapsing matter enters the near-horizon region, despite the absence of large curvature invariants. Within the scrambling time, the uneventful horizon transitions towards a firewall, and eventually the effective field theory breaks down.