{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:4C5FFNTMSSNQEPMJ3MTMBQMBV2","short_pith_number":"pith:4C5FFNTM","schema_version":"1.0","canonical_sha256":"e0ba52b66c949b023d89db26c0c181aea720c6fbee7ae7724cd393d71657b9e6","source":{"kind":"arxiv","id":"2306.16469","version":2},"attestation_state":"computed","paper":{"title":"Recipes for computing radiation from a Kerr black hole using a generalized Sasaki-Nakamura formalism: Homogeneous solutions","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Rico K. L. Lo","submitted_at":"2023-06-28T18:00:39Z","abstract_excerpt":"Central to black hole perturbation theory calculations is the Teukolsky equation that governs the propagation and the generation of radiation emitted by Kerr black holes. However, it is plagued by a long-ranged potential associated with the perturbation equation and hence a direct numerical integration of the equation is challenging. Sasaki and Nakamura devised a formulation that transforms the equation into a new equation that is free from the issue for the case of outgoing gravitational radiation. The formulation was later generalized by Hughes to work for any type of radiation. In this work"},"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":"2306.16469","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"gr-qc","submitted_at":"2023-06-28T18:00:39Z","cross_cats_sorted":[],"title_canon_sha256":"1ef8e7bc99ce50b3c8dc798d939e84ee228e8da9d9675c7e8ed976fb5747381e","abstract_canon_sha256":"34d6d84edcc167a02616a83584b445f5f97b772e210fc5c8da845908720fde63"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T09:56:20.082678Z","signature_b64":"k003P5gqRZ6np3dSLze+p5IhWlKnY2iuJirgfOsDrsEWx/lddZJpmGp3gS4uFg4BsVsBFAsjZBIksCcuSvd+BA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"e0ba52b66c949b023d89db26c0c181aea720c6fbee7ae7724cd393d71657b9e6","last_reissued_at":"2026-07-05T09:56:20.082327Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T09:56:20.082327Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Recipes for computing radiation from a Kerr black hole using a generalized Sasaki-Nakamura formalism: Homogeneous solutions","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Rico K. L. Lo","submitted_at":"2023-06-28T18:00:39Z","abstract_excerpt":"Central to black hole perturbation theory calculations is the Teukolsky equation that governs the propagation and the generation of radiation emitted by Kerr black holes. However, it is plagued by a long-ranged potential associated with the perturbation equation and hence a direct numerical integration of the equation is challenging. Sasaki and Nakamura devised a formulation that transforms the equation into a new equation that is free from the issue for the case of outgoing gravitational radiation. The formulation was later generalized by Hughes to work for any type of radiation. In this work"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2306.16469","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/2306.16469/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":"2306.16469","created_at":"2026-07-05T09:56:20.082385+00:00"},{"alias_kind":"arxiv_version","alias_value":"2306.16469v2","created_at":"2026-07-05T09:56:20.082385+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2306.16469","created_at":"2026-07-05T09:56:20.082385+00:00"},{"alias_kind":"pith_short_12","alias_value":"4C5FFNTMSSNQ","created_at":"2026-07-05T09:56:20.082385+00:00"},{"alias_kind":"pith_short_16","alias_value":"4C5FFNTMSSNQEPMJ","created_at":"2026-07-05T09:56:20.082385+00:00"},{"alias_kind":"pith_short_8","alias_value":"4C5FFNTM","created_at":"2026-07-05T09:56:20.082385+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2605.09250","citing_title":"Efficient and Stable Computation of Gravitational-Wave Fluxes from Generic Kerr Orbits via a Unified HeunC Framework","ref_index":83,"is_internal_anchor":false},{"citing_arxiv_id":"2512.23510","citing_title":"Quasinormal mode/grey-body factor correspondence for Kerr black holes","ref_index":65,"is_internal_anchor":false},{"citing_arxiv_id":"2605.09250","citing_title":"Efficient and Stable Computation of Gravitational-Wave Fluxes from Generic Kerr Orbits via a Unified HeunC Framework","ref_index":83,"is_internal_anchor":false},{"citing_arxiv_id":"2605.09250","citing_title":"Efficient and Stable Computation of Gravitational-Wave Fluxes from Generic Kerr Orbits via a Unified HeunC Framework","ref_index":83,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/4C5FFNTMSSNQEPMJ3MTMBQMBV2","json":"https://pith.science/pith/4C5FFNTMSSNQEPMJ3MTMBQMBV2.json","graph_json":"https://pith.science/api/pith-number/4C5FFNTMSSNQEPMJ3MTMBQMBV2/graph.json","events_json":"https://pith.science/api/pith-number/4C5FFNTMSSNQEPMJ3MTMBQMBV2/events.json","paper":"https://pith.science/paper/4C5FFNTM"},"agent_actions":{"view_html":"https://pith.science/pith/4C5FFNTMSSNQEPMJ3MTMBQMBV2","download_json":"https://pith.science/pith/4C5FFNTMSSNQEPMJ3MTMBQMBV2.json","view_paper":"https://pith.science/paper/4C5FFNTM","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2306.16469&json=true","fetch_graph":"https://pith.science/api/pith-number/4C5FFNTMSSNQEPMJ3MTMBQMBV2/graph.json","fetch_events":"https://pith.science/api/pith-number/4C5FFNTMSSNQEPMJ3MTMBQMBV2/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/4C5FFNTMSSNQEPMJ3MTMBQMBV2/action/timestamp_anchor","attest_storage":"https://pith.science/pith/4C5FFNTMSSNQEPMJ3MTMBQMBV2/action/storage_attestation","attest_author":"https://pith.science/pith/4C5FFNTMSSNQEPMJ3MTMBQMBV2/action/author_attestation","sign_citation":"https://pith.science/pith/4C5FFNTMSSNQEPMJ3MTMBQMBV2/action/citation_signature","submit_replication":"https://pith.science/pith/4C5FFNTMSSNQEPMJ3MTMBQMBV2/action/replication_record"}},"created_at":"2026-07-05T09:56:20.082385+00:00","updated_at":"2026-07-05T09:56:20.082385+00:00"}