{"paper":{"title":"Electromagnetic Emission from a Black Hole Evaporating in External Magnetic Field","arxiv_id":"2607.16880","primary_cat":"astro-ph.HE","submitted_at":"2026-07-18T16:39:06+00:00","version_compiled":"v1"},"notice":"Every quoted sentence is the authors' text from the arXiv listing abstract. Labels and probabilities are the outputs of classifier-1.13.0 on the question bank abstract-p1-20260923, exactly as returned. 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effect.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.71,"main_claim_p":0.17,"quantitative":false,"quantitative_p":0.28,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.66,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.11,"interpretation":0.23}},{"i":2,"p":0.59,"id":"s2","own":true,"role":"interpretation","text":"The time evolution of the spacetime metric perturbs a static background magnetic field, inducing a radiative field that acts as an effective electromagnetic source even in the absence of physical charges or currents.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.74,"main_claim_p":0.34,"quantitative":false,"quantitative_p":0.04,"role_probabilities":{"gap":0.0,"method":0.03,"result":0.12,"background":0.01,"limitation":0.0,"future_work":0.0,"contribution":0.25,"interpretation":0.59}},{"i":3,"p":1.0,"id":"s3","own":true,"role":"method","text":"To isolate the dynamic effects of the time-dependent spacetime on the external magnetic field, we approximate Hawking radiation as a spherically symmetric outflow of null fluid governed by the prescribed time-dependence of the central mass $M(t)$.","hedge":{"p":0.98,"label":"asserted"},"own_p":0.88,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.07,"role_probabilities":{"gap":0.0,"method":1.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":4,"p":1.0,"id":"s4","own":true,"role":"method","text":"We employ Laplace transform, which selects the retarded outgoing branch of the electromagnetic response, producing fields proportional to $\\Theta(t-r)$ and thereby fixing a causal radiative arrow of emission.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.92,"main_claim_p":0.04,"quantitative":false,"quantitative_p":0.07,"role_probabilities":{"gap":0.0,"method":1.0,"result":0.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":5,"p":1.0,"id":"s5","own":true,"role":"result","text":"The emitted spectral energy is red-dominated, scaling as $d\\mathcal{E}_B/d\\omega \\propto B_0^2 m_0^2 \\tau_H^{-2/3} \\omega^{-8/3}$, where $\\tau_H$ is the Hawking evaporation timescale, and corresponds to a pure Transverse Electric (TE) mode.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.91,"main_claim_p":0.35,"quantitative":true,"quantitative_p":0.85,"role_probabilities":{"gap":0.0,"method":0.0,"result":1.0,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.0}},{"i":6,"p":1.0,"id":"s6","own":true,"role":"result","text":"There is no final bright burst at the end of the 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