{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:SQTTWGCGTKS732HUYHJQ23V2QN","short_pith_number":"pith:SQTTWGCG","schema_version":"1.0","canonical_sha256":"94273b18469aa5fde8f4c1d30d6eba8355a3689f6a00b8757184110fc1832837","source":{"kind":"arxiv","id":"1702.00872","version":2},"attestation_state":"computed","paper":{"title":"Post-Newtonian Quasicircular Initial Orbits for Numerical Relativity","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"gr-qc","authors_text":"Carlos O. Lousto, Hiroyuki Nakano, James Healy, Yosef Zlochower","submitted_at":"2017-02-02T23:48:41Z","abstract_excerpt":"We use post-Newtonian (PN) approximations to determine the initial orbital and spin parameters of black hole binaries that lead to low-eccentricity inspirals when evolved with numerical relativity techniques. In particular, we seek initial configurations that lead to very small eccentricities at small separations, as is expected for astrophysical systems. We consider three cases: (i) quasicircular orbits with no radial velocity, (ii) quasicircular orbits with an initial radial velocity determined by radiation reaction, and (iii) parameters obtained form evolution of the PN equations of motion "},"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":"1702.00872","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"gr-qc","submitted_at":"2017-02-02T23:48:41Z","cross_cats_sorted":["astro-ph.CO"],"title_canon_sha256":"d741d4d3f85fa3c57c395d817cf282176afa1c237ca5438efc1ecfba31827e5d","abstract_canon_sha256":"e60ce9d30d740755a418303205507a71a3ecf35b0464335815ea680092b9f1a7"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T01:49:44.806805Z","signature_b64":"SccGxTEpSrL0JK24ZRW2aHvWg0nGnD/2uF0CXNQsyGfposNTzzamJkrpNPHwpVRGQ1lKIEgYW0bVdFdGs6iKAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"94273b18469aa5fde8f4c1d30d6eba8355a3689f6a00b8757184110fc1832837","last_reissued_at":"2026-07-05T01:49:44.806304Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T01:49:44.806304Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Post-Newtonian Quasicircular Initial Orbits for Numerical Relativity","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"gr-qc","authors_text":"Carlos O. Lousto, Hiroyuki Nakano, James Healy, Yosef Zlochower","submitted_at":"2017-02-02T23:48:41Z","abstract_excerpt":"We use post-Newtonian (PN) approximations to determine the initial orbital and spin parameters of black hole binaries that lead to low-eccentricity inspirals when evolved with numerical relativity techniques. In particular, we seek initial configurations that lead to very small eccentricities at small separations, as is expected for astrophysical systems. We consider three cases: (i) quasicircular orbits with no radial velocity, (ii) quasicircular orbits with an initial radial velocity determined by radiation reaction, and (iii) parameters obtained form evolution of the PN equations of motion "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1702.00872","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/1702.00872/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":"1702.00872","created_at":"2026-07-05T01:49:44.806371+00:00"},{"alias_kind":"arxiv_version","alias_value":"1702.00872v2","created_at":"2026-07-05T01:49:44.806371+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1702.00872","created_at":"2026-07-05T01:49:44.806371+00:00"},{"alias_kind":"pith_short_12","alias_value":"SQTTWGCGTKS7","created_at":"2026-07-05T01:49:44.806371+00:00"},{"alias_kind":"pith_short_16","alias_value":"SQTTWGCGTKS732HU","created_at":"2026-07-05T01:49:44.806371+00:00"},{"alias_kind":"pith_short_8","alias_value":"SQTTWGCG","created_at":"2026-07-05T01:49:44.806371+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2507.22862","citing_title":"Parameter Estimation with Targeted Eccentric Numerical-Relativity Simulations for GW200208_22 and GW190620","ref_index":90,"is_internal_anchor":false},{"citing_arxiv_id":"2508.21216","citing_title":"Persistence of post-Newtonian amplitude structure in binary black hole mergers","ref_index":54,"is_internal_anchor":false},{"citing_arxiv_id":"2604.17868","citing_title":"Including higher-order modes in a quadrupolar eccentric numerical relativity surrogate using universal eccentric modulation functions","ref_index":32,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/SQTTWGCGTKS732HUYHJQ23V2QN","json":"https://pith.science/pith/SQTTWGCGTKS732HUYHJQ23V2QN.json","graph_json":"https://pith.science/api/pith-number/SQTTWGCGTKS732HUYHJQ23V2QN/graph.json","events_json":"https://pith.science/api/pith-number/SQTTWGCGTKS732HUYHJQ23V2QN/events.json","paper":"https://pith.science/paper/SQTTWGCG"},"agent_actions":{"view_html":"https://pith.science/pith/SQTTWGCGTKS732HUYHJQ23V2QN","download_json":"https://pith.science/pith/SQTTWGCGTKS732HUYHJQ23V2QN.json","view_paper":"https://pith.science/paper/SQTTWGCG","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1702.00872&json=true","fetch_graph":"https://pith.science/api/pith-number/SQTTWGCGTKS732HUYHJQ23V2QN/graph.json","fetch_events":"https://pith.science/api/pith-number/SQTTWGCGTKS732HUYHJQ23V2QN/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/SQTTWGCGTKS732HUYHJQ23V2QN/action/timestamp_anchor","attest_storage":"https://pith.science/pith/SQTTWGCGTKS732HUYHJQ23V2QN/action/storage_attestation","attest_author":"https://pith.science/pith/SQTTWGCGTKS732HUYHJQ23V2QN/action/author_attestation","sign_citation":"https://pith.science/pith/SQTTWGCGTKS732HUYHJQ23V2QN/action/citation_signature","submit_replication":"https://pith.science/pith/SQTTWGCGTKS732HUYHJQ23V2QN/action/replication_record"}},"created_at":"2026-07-05T01:49:44.806371+00:00","updated_at":"2026-07-05T01:49:44.806371+00:00"}