{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:FPKM2L4I7DM3V4Z2YFC62D2KYB","short_pith_number":"pith:FPKM2L4I","schema_version":"1.0","canonical_sha256":"2bd4cd2f88f8d9baf33ac145ed0f4ac071fc38b969f0313a0d6949546d21a86b","source":{"kind":"arxiv","id":"1910.13452","version":2},"attestation_state":"computed","paper":{"title":"Hyperboloidal framework for the Kerr spacetime","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Rodrigo Panosso Macedo","submitted_at":"2019-10-29T18:00:02Z","abstract_excerpt":"Motivated by the need of a robust geometrical framework for the calculation of long, and highly accurate waveforms for extreme-mass-ratio inspirals, this work presents an extensive study of the hyperboloidal formalism for the Kerr spacetime and the Teukolsky equation. In a first step, we introduce a generic coordinate system foliating the Kerr spacetime into hypersurfaces of constant time extending between the black-hole horizon and future null infinity, while keeping track of the underlying degrees of freedom. Then, we express the Teukolsky equation in terms of these generic coordinates with "},"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":"1910.13452","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2019-10-29T18:00:02Z","cross_cats_sorted":[],"title_canon_sha256":"4aede48c9e1ca896d2e06ba7491cb8d6c2809eccf450a174f05f8cdcb2a49317","abstract_canon_sha256":"9f3375949924dd79362f368975f213eb31318db296f655167ae1b34ba1e56cfe"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T00:46:04.809433Z","signature_b64":"vdO4wUJZ2vTeuOCZXB+iLDYwaO0h7la2kTjuTFl5QtaKuSfHiSdNuEKzzY02dtxvjE9uxYYnHmHPLmQDS07vAA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"2bd4cd2f88f8d9baf33ac145ed0f4ac071fc38b969f0313a0d6949546d21a86b","last_reissued_at":"2026-07-05T00:46:04.808959Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T00:46:04.808959Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Hyperboloidal framework for the Kerr spacetime","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Rodrigo Panosso Macedo","submitted_at":"2019-10-29T18:00:02Z","abstract_excerpt":"Motivated by the need of a robust geometrical framework for the calculation of long, and highly accurate waveforms for extreme-mass-ratio inspirals, this work presents an extensive study of the hyperboloidal formalism for the Kerr spacetime and the Teukolsky equation. In a first step, we introduce a generic coordinate system foliating the Kerr spacetime into hypersurfaces of constant time extending between the black-hole horizon and future null infinity, while keeping track of the underlying degrees of freedom. Then, we express the Teukolsky equation in terms of these generic coordinates with "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1910.13452","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/1910.13452/integrity.json","findings":[],"available":true,"detectors_run":[],"snapshot_sha256":"c28c3603d3b5d939e8dc4c7e95fa8dfce3d595e45f758748cecf8e644a296938"},"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":"1910.13452","created_at":"2026-07-05T00:46:04.809018+00:00"},{"alias_kind":"arxiv_version","alias_value":"1910.13452v2","created_at":"2026-07-05T00:46:04.809018+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1910.13452","created_at":"2026-07-05T00:46:04.809018+00:00"},{"alias_kind":"pith_short_12","alias_value":"FPKM2L4I7DM3","created_at":"2026-07-05T00:46:04.809018+00:00"},{"alias_kind":"pith_short_16","alias_value":"FPKM2L4I7DM3V4Z2","created_at":"2026-07-05T00:46:04.809018+00:00"},{"alias_kind":"pith_short_8","alias_value":"FPKM2L4I","created_at":"2026-07-05T00:46:04.809018+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.26339","citing_title":"Time-domain framework for the Teukolsky equation with a particle source using comoving hyperboloidal coordinates","ref_index":48,"is_internal_anchor":false},{"citing_arxiv_id":"2510.27320","citing_title":"The quasinormal modes of the rotating quantum corrected black holes","ref_index":38,"is_internal_anchor":false},{"citing_arxiv_id":"2604.22734","citing_title":"Radiation outer boundary conditions and near-to-far field signal transformations for the Bardeen-Press equation","ref_index":45,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/FPKM2L4I7DM3V4Z2YFC62D2KYB","json":"https://pith.science/pith/FPKM2L4I7DM3V4Z2YFC62D2KYB.json","graph_json":"https://pith.science/api/pith-number/FPKM2L4I7DM3V4Z2YFC62D2KYB/graph.json","events_json":"https://pith.science/api/pith-number/FPKM2L4I7DM3V4Z2YFC62D2KYB/events.json","paper":"https://pith.science/paper/FPKM2L4I"},"agent_actions":{"view_html":"https://pith.science/pith/FPKM2L4I7DM3V4Z2YFC62D2KYB","download_json":"https://pith.science/pith/FPKM2L4I7DM3V4Z2YFC62D2KYB.json","view_paper":"https://pith.science/paper/FPKM2L4I","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1910.13452&json=true","fetch_graph":"https://pith.science/api/pith-number/FPKM2L4I7DM3V4Z2YFC62D2KYB/graph.json","fetch_events":"https://pith.science/api/pith-number/FPKM2L4I7DM3V4Z2YFC62D2KYB/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/FPKM2L4I7DM3V4Z2YFC62D2KYB/action/timestamp_anchor","attest_storage":"https://pith.science/pith/FPKM2L4I7DM3V4Z2YFC62D2KYB/action/storage_attestation","attest_author":"https://pith.science/pith/FPKM2L4I7DM3V4Z2YFC62D2KYB/action/author_attestation","sign_citation":"https://pith.science/pith/FPKM2L4I7DM3V4Z2YFC62D2KYB/action/citation_signature","submit_replication":"https://pith.science/pith/FPKM2L4I7DM3V4Z2YFC62D2KYB/action/replication_record"}},"created_at":"2026-07-05T00:46:04.809018+00:00","updated_at":"2026-07-05T00:46:04.809018+00:00"}