{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2002:E6NFW7NG6XEUDS4OONH4GQ2672","short_pith_number":"pith:E6NFW7NG","schema_version":"1.0","canonical_sha256":"279a5b7da6f5c941cb8e734fc3435efeb24278f5cf6c1542c2783172c491072e","source":{"kind":"arxiv","id":"gr-qc/0208089","version":2},"attestation_state":"computed","paper":{"title":"Numerically generated quasi-equilibrium orbits of black holes: Circular or eccentric?","license":"","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Clifford M. Will (Washington University, Paris), St. Louis), Thierry Mora (Ecole Normale Superieure","submitted_at":"2002-08-29T15:16:08Z","abstract_excerpt":"We make a comparison between results from numerically generated, quasi-equilibrium configurations of compact binary systems of black holes in close orbits, and results from the post-Newtonian approximation. The post-Newtonian results are accurate through third PN order (O(v/c)^6 beyond Newtonian gravity), and include rotational and spin-orbit effects, but are generalized to permit orbits of non-zero eccentricity. Both treatments ignore gravitational radiation reaction. The energy E and angular momentum J of a given configuration are compared between the two methods as a function of the orbital"},"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":"gr-qc/0208089","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"gr-qc","submitted_at":"2002-08-29T15:16:08Z","cross_cats_sorted":[],"title_canon_sha256":"e1963a12570bcf52addafd4db02ab9fb3d9f1f682fa7cd1478aad8f81c6f0154","abstract_canon_sha256":"1bb12ad44326e47fcfa741a4cec86e053b167b2355d6b39e7dde445b5383f881"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:33:46.393097Z","signature_b64":"/ooQLPrbiuO2TNxJAGHRjK/oO4a8HA1HJVVFpi/UOczXJ8ka+P9sAlDXJynMOL9ho3HSuMeTIbkRrM1v/bSnCg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"279a5b7da6f5c941cb8e734fc3435efeb24278f5cf6c1542c2783172c491072e","last_reissued_at":"2026-07-04T16:33:46.392647Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:33:46.392647Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Numerically generated quasi-equilibrium orbits of black holes: Circular or eccentric?","license":"","headline":"","cross_cats":[],"primary_cat":"gr-qc","authors_text":"Clifford M. Will (Washington University, Paris), St. Louis), Thierry Mora (Ecole Normale Superieure","submitted_at":"2002-08-29T15:16:08Z","abstract_excerpt":"We make a comparison between results from numerically generated, quasi-equilibrium configurations of compact binary systems of black holes in close orbits, and results from the post-Newtonian approximation. The post-Newtonian results are accurate through third PN order (O(v/c)^6 beyond Newtonian gravity), and include rotational and spin-orbit effects, but are generalized to permit orbits of non-zero eccentricity. Both treatments ignore gravitational radiation reaction. The energy E and angular momentum J of a given configuration are compared between the two methods as a function of the orbital"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"gr-qc/0208089","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/gr-qc/0208089/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":"gr-qc/0208089","created_at":"2026-07-04T16:33:46.392709+00:00"},{"alias_kind":"arxiv_version","alias_value":"gr-qc/0208089v2","created_at":"2026-07-04T16:33:46.392709+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.gr-qc/0208089","created_at":"2026-07-04T16:33:46.392709+00:00"},{"alias_kind":"pith_short_12","alias_value":"E6NFW7NG6XEU","created_at":"2026-07-04T16:33:46.392709+00:00"},{"alias_kind":"pith_short_16","alias_value":"E6NFW7NG6XEUDS4O","created_at":"2026-07-04T16:33:46.392709+00:00"},{"alias_kind":"pith_short_8","alias_value":"E6NFW7NG","created_at":"2026-07-04T16:33:46.392709+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2502.06952","citing_title":"Non-adiabatic dynamics of eccentric black-hole binaries in post-Newtonian theory","ref_index":29,"is_internal_anchor":true},{"citing_arxiv_id":"2604.15431","citing_title":"Highly eccentric non-spinning binary black hole mergers: quadrupolar post-merger waveforms","ref_index":150,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/E6NFW7NG6XEUDS4OONH4GQ2672","json":"https://pith.science/pith/E6NFW7NG6XEUDS4OONH4GQ2672.json","graph_json":"https://pith.science/api/pith-number/E6NFW7NG6XEUDS4OONH4GQ2672/graph.json","events_json":"https://pith.science/api/pith-number/E6NFW7NG6XEUDS4OONH4GQ2672/events.json","paper":"https://pith.science/paper/E6NFW7NG"},"agent_actions":{"view_html":"https://pith.science/pith/E6NFW7NG6XEUDS4OONH4GQ2672","download_json":"https://pith.science/pith/E6NFW7NG6XEUDS4OONH4GQ2672.json","view_paper":"https://pith.science/paper/E6NFW7NG","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=gr-qc/0208089&json=true","fetch_graph":"https://pith.science/api/pith-number/E6NFW7NG6XEUDS4OONH4GQ2672/graph.json","fetch_events":"https://pith.science/api/pith-number/E6NFW7NG6XEUDS4OONH4GQ2672/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/E6NFW7NG6XEUDS4OONH4GQ2672/action/timestamp_anchor","attest_storage":"https://pith.science/pith/E6NFW7NG6XEUDS4OONH4GQ2672/action/storage_attestation","attest_author":"https://pith.science/pith/E6NFW7NG6XEUDS4OONH4GQ2672/action/author_attestation","sign_citation":"https://pith.science/pith/E6NFW7NG6XEUDS4OONH4GQ2672/action/citation_signature","submit_replication":"https://pith.science/pith/E6NFW7NG6XEUDS4OONH4GQ2672/action/replication_record"}},"created_at":"2026-07-04T16:33:46.392709+00:00","updated_at":"2026-07-04T16:33:46.392709+00:00"}