{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2011:BJSSZQ44ELG6B4FUYJ7AYCOI22","short_pith_number":"pith:BJSSZQ44","schema_version":"1.0","canonical_sha256":"0a652cc39c22cde0f0b4c27e0c09c8d6ade5627aeea40951047f1ba5125d7f31","source":{"kind":"arxiv","id":"1105.3191","version":2},"attestation_state":"computed","paper":{"title":"A Metric for Rapidly Spinning Black Holes Suitable for Strong-Field Tests of the No-Hair Theorem","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"gr-qc","authors_text":"Dimitrios Psaltis (Arizona), Tim Johannsen","submitted_at":"2011-05-16T20:00:02Z","abstract_excerpt":"According to the no-hair theorem, astrophysical black holes are uniquely characterized by their masses and spins and are described by the Kerr metric. Several parametric deviations from the Kerr metric have been suggested to study observational signatures in both the electromagnetic and gravitational-wave spectra that differ from the expected Kerr signals. Due to the no-hair theorem, however, such spacetimes cannot be regular everywhere outside the event horizons, if they are solutions to the Einstein field equations; they are often characterized by naked singularities or closed time-like loop"},"verification_status":{"content_addressed":true,"pith_receipt":true,"author_attested":false,"weak_author_claims":0,"strong_author_claims":0,"externally_anchored":false,"storage_verified":false,"citation_signatures":0,"replication_records":0,"graph_snapshot":true,"references_resolved":false,"formal_links_present":false},"canonical_record":{"source":{"id":"1105.3191","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2011-05-16T20:00:02Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"eb9efdd5fd7eafee9536cf8ca9fd3471d058d4996ad949f4bc1e6e8aac58186c","abstract_canon_sha256":"1de3331405cea7b8966619695f3bfdf5e9806d8ca1113cfd19682ce9c3f2d0df"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T04:19:31.878665Z","signature_b64":"Jl6lA85OgfDEXeQ6ELHyOSWjt0u8CniA7VPkr+ks9JlFC0xGqV0nDZ9CNL6i9Uo6gP2i+gS+qprg1ucactmHBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"0a652cc39c22cde0f0b4c27e0c09c8d6ade5627aeea40951047f1ba5125d7f31","last_reissued_at":"2026-05-18T04:19:31.878211Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T04:19:31.878211Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A Metric for Rapidly Spinning Black Holes Suitable for Strong-Field Tests of the No-Hair Theorem","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"gr-qc","authors_text":"Dimitrios Psaltis (Arizona), Tim Johannsen","submitted_at":"2011-05-16T20:00:02Z","abstract_excerpt":"According to the no-hair theorem, astrophysical black holes are uniquely characterized by their masses and spins and are described by the Kerr metric. Several parametric deviations from the Kerr metric have been suggested to study observational signatures in both the electromagnetic and gravitational-wave spectra that differ from the expected Kerr signals. Due to the no-hair theorem, however, such spacetimes cannot be regular everywhere outside the event horizons, if they are solutions to the Einstein field equations; they are often characterized by naked singularities or closed time-like loop"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1105.3191","kind":"arxiv","version":2},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"},"aliases":[{"alias_kind":"arxiv","alias_value":"1105.3191","created_at":"2026-05-18T04:19:31.878292+00:00"},{"alias_kind":"arxiv_version","alias_value":"1105.3191v2","created_at":"2026-05-18T04:19:31.878292+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1105.3191","created_at":"2026-05-18T04:19:31.878292+00:00"},{"alias_kind":"pith_short_12","alias_value":"BJSSZQ44ELG6","created_at":"2026-05-18T12:26:24.575870+00:00"},{"alias_kind":"pith_short_16","alias_value":"BJSSZQ44ELG6B4FU","created_at":"2026-05-18T12:26:24.575870+00:00"},{"alias_kind":"pith_short_8","alias_value":"BJSSZQ44","created_at":"2026-05-18T12:26:24.575870+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":6,"internal_anchor_count":5,"sample":[{"citing_arxiv_id":"2605.20524","citing_title":"Light Deflection due to Spinoptic Effects in Parametrized and Spherically Symmetric Hairy Black Holes","ref_index":25,"is_internal_anchor":true},{"citing_arxiv_id":"2605.19463","citing_title":"Memory burden effect of regular primordial black holes","ref_index":82,"is_internal_anchor":true},{"citing_arxiv_id":"2601.09607","citing_title":"Confronting eikonal and post-Kerr methods with numerical evolution of scalar field perturbations in spacetimes beyond Kerr","ref_index":55,"is_internal_anchor":true},{"citing_arxiv_id":"2601.22914","citing_title":"Exact black holes and black branes with bumpy horizons supported by superfluid pions","ref_index":33,"is_internal_anchor":true},{"citing_arxiv_id":"2602.16237","citing_title":"Rotating Black Holes with Primary Scalar Hair: Shadow Signatures in Beyond Horndeski Gravity","ref_index":86,"is_internal_anchor":true},{"citing_arxiv_id":"2605.05352","citing_title":"Perturbations in the parametrized wormhole spacetime and their related quasinormal modes","ref_index":39,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/BJSSZQ44ELG6B4FUYJ7AYCOI22","json":"https://pith.science/pith/BJSSZQ44ELG6B4FUYJ7AYCOI22.json","graph_json":"https://pith.science/api/pith-number/BJSSZQ44ELG6B4FUYJ7AYCOI22/graph.json","events_json":"https://pith.science/api/pith-number/BJSSZQ44ELG6B4FUYJ7AYCOI22/events.json","paper":"https://pith.science/paper/BJSSZQ44"},"agent_actions":{"view_html":"https://pith.science/pith/BJSSZQ44ELG6B4FUYJ7AYCOI22","download_json":"https://pith.science/pith/BJSSZQ44ELG6B4FUYJ7AYCOI22.json","view_paper":"https://pith.science/paper/BJSSZQ44","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1105.3191&json=true","fetch_graph":"https://pith.science/api/pith-number/BJSSZQ44ELG6B4FUYJ7AYCOI22/graph.json","fetch_events":"https://pith.science/api/pith-number/BJSSZQ44ELG6B4FUYJ7AYCOI22/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/BJSSZQ44ELG6B4FUYJ7AYCOI22/action/timestamp_anchor","attest_storage":"https://pith.science/pith/BJSSZQ44ELG6B4FUYJ7AYCOI22/action/storage_attestation","attest_author":"https://pith.science/pith/BJSSZQ44ELG6B4FUYJ7AYCOI22/action/author_attestation","sign_citation":"https://pith.science/pith/BJSSZQ44ELG6B4FUYJ7AYCOI22/action/citation_signature","submit_replication":"https://pith.science/pith/BJSSZQ44ELG6B4FUYJ7AYCOI22/action/replication_record"}},"created_at":"2026-05-18T04:19:31.878292+00:00","updated_at":"2026-05-18T04:19:31.878292+00:00"}