{"paper":{"title":"Energy and angular momentum of charged rotating black holes","arxiv_id":"gr-qc/9501002","primary_cat":"gr-qc","submitted_at":"1995-01-03T14:44:00+00:00","version_compiled":"v3"},"notice":"Every quoted sentence is the authors' text from the arXiv listing abstract. Labels and probabilities are the outputs of classifier-1.13-20260917 on the question bank abstract-p1-20260923, exactly as returned. No sentence in this record was written by a language model.","schema":"pith.compiled-record/v0","status":"compiled","abstract":{"source":"arXiv listing abstract v3","sentences":[{"i":0,"p":0.91,"id":"s0","own":true,"role":"result","text":"We show that the pseudotensors of Einstein, Tolman, Landau and Lifshitz, Papapetrou, and Weinberg (ETLLPW) give the same distributions of energy, linear momentum and angular momentum, for any Kerr-Schild metric.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.93,"main_claim_p":0.87,"quantitative":false,"quantitative_p":0.48,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.91,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.09,"interpretation":0.0}},{"i":1,"p":0.63,"id":"s1","own":false,"role":"background","text":"This result generalizes a previous work by G\\\"urses and G\\\"ursey that dealt only with the pseudotensors of Einstein and Landau and Lifshitz.","hedge":{"p":0.99,"label":"asserted"},"own_p":0.15,"main_claim_p":0.06,"quantitative":false,"quantitative_p":0.22,"role_probabilities":{"gap":0.16,"method":0.0,"result":0.03,"background":0.63,"limitation":0.0,"future_work":0.0,"contribution":0.15,"interpretation":0.03}},{"i":2,"p":0.61,"id":"s2","own":true,"role":"result","text":"We compute these distributions for the Kerr-Newman and Bonnor-Vaidya metrics and find reasonable results.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.97,"main_claim_p":0.1,"quantitative":false,"quantitative_p":0.06,"role_probabilities":{"gap":0.0,"method":0.01,"result":0.61,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.38,"interpretation":0.0}},{"i":3,"p":1.0,"id":"s3","own":true,"role":"method","text":"All calculations are performed without any approximation in Kerr-Schild Cartesian coordinates.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.94,"main_claim_p":0.03,"quantitative":false,"quantitative_p":0.08,"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":"result","text":"For the Reissner-Nordstr\\\"{o}m metric these definitions give the same result as the Penrose quasi-local mass.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.8,"main_claim_p":0.07,"quantitative":true,"quantitative_p":0.6,"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":5,"p":0.93,"id":"s5","own":true,"role":"result","text":"For the Kerr black hole the entire energy is confined to its interior whereas for the Kerr-Newman black hole, as expected, the energy is shared by its interior as well as exterior.","hedge":{"p":1.0,"label":"asserted"},"own_p":0.89,"main_claim_p":0.09,"quantitative":true,"quantitative_p":0.54,"role_probabilities":{"gap":0.0,"method":0.0,"result":0.93,"background":0.0,"limitation":0.0,"future_work":0.0,"contribution":0.0,"interpretation":0.07}},{"i":6,"p":1.0,"id":"s6","own":true,"role":"result","text":"The total energy and angular momentum of the Kerr-Newman black hole are $M$ and $ M a$, respectively ($M$ is the mass parameter and $a$ is the rotation parameter).","hedge":{"p":1.0,"label":"asserted"},"own_p":0.9,"main_claim_p":0.15,"quantitative":true,"quantitative_p":0.58,"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":7,"p":1.0,"id":"s7","own":true,"role":"result","text":"The energy distribution for the Bonnor-Vaidya metric is the same as the Penrose quasi-local mass obtained by 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