{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:1999:IY5M4ZGFOEEQFAIHN6DUOOCITS","short_pith_number":"pith:IY5M4ZGF","schema_version":"1.0","canonical_sha256":"463ace64c571090281076f874738489cbf3e495d396e7ebb97d64c0518321b40","source":{"kind":"arxiv","id":"astro-ph/9909073","version":1},"attestation_state":"computed","paper":{"title":"Tidal evolution of eccentric orbits in massive binary systems; a study of resonance locking","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"G.J. Savonije (University of Amsterdam), M.G. Witte","submitted_at":"1999-09-03T16:32:49Z","abstract_excerpt":"We study the tidal evolution of a binary system consisting of a 1.4 Msun compact object in elliptic orbit about a 10 Msun uniformly rotating main sequence star for various values of the initial orbital parameters. We apply our previously published results of 2D non-adiabatic calculations of the non-radial g- and r-mode oscillations of the uniformly rotating MS star, and include the effects of resonant excitation of these modes in the tidal evolution calculations. A high orbital eccentricity enhances the effectiveness of the tidal interaction because of the large number of harmonic components o"},"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":"astro-ph/9909073","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"1999-09-03T16:32:49Z","cross_cats_sorted":[],"title_canon_sha256":"ccc73d12558075fb124ad26aeed0af73505a6375d2dd1bf506542e1736c0e540","abstract_canon_sha256":"0bab71ac069013b22455015d530c94fda14bcc27e68c62b8b6cffb7544e09a8d"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T14:17:05.342853Z","signature_b64":"68TEUG5Gipkmgut4CrUHXDX1gSFrtXYfvmdYQp51lHurEZMvGwck1+39PMQJOZ3+Kema9c9eq7jGR7px/XSfAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"463ace64c571090281076f874738489cbf3e495d396e7ebb97d64c0518321b40","last_reissued_at":"2026-07-04T14:17:05.342306Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T14:17:05.342306Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Tidal evolution of eccentric orbits in massive binary systems; a study of resonance locking","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"G.J. Savonije (University of Amsterdam), M.G. Witte","submitted_at":"1999-09-03T16:32:49Z","abstract_excerpt":"We study the tidal evolution of a binary system consisting of a 1.4 Msun compact object in elliptic orbit about a 10 Msun uniformly rotating main sequence star for various values of the initial orbital parameters. We apply our previously published results of 2D non-adiabatic calculations of the non-radial g- and r-mode oscillations of the uniformly rotating MS star, and include the effects of resonant excitation of these modes in the tidal evolution calculations. A high orbital eccentricity enhances the effectiveness of the tidal interaction because of the large number of harmonic components o"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/9909073","kind":"arxiv","version":1},"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/astro-ph/9909073/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":"astro-ph/9909073","created_at":"2026-07-04T14:17:05.342376+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/9909073v1","created_at":"2026-07-04T14:17:05.342376+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/9909073","created_at":"2026-07-04T14:17:05.342376+00:00"},{"alias_kind":"pith_short_12","alias_value":"IY5M4ZGFOEEQ","created_at":"2026-07-04T14:17:05.342376+00:00"},{"alias_kind":"pith_short_16","alias_value":"IY5M4ZGFOEEQFAIH","created_at":"2026-07-04T14:17:05.342376+00:00"},{"alias_kind":"pith_short_8","alias_value":"IY5M4ZGF","created_at":"2026-07-04T14:17:05.342376+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2501.13929","citing_title":"Testing tidal theory using Gaia binaries: the red giant branch","ref_index":50,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/IY5M4ZGFOEEQFAIHN6DUOOCITS","json":"https://pith.science/pith/IY5M4ZGFOEEQFAIHN6DUOOCITS.json","graph_json":"https://pith.science/api/pith-number/IY5M4ZGFOEEQFAIHN6DUOOCITS/graph.json","events_json":"https://pith.science/api/pith-number/IY5M4ZGFOEEQFAIHN6DUOOCITS/events.json","paper":"https://pith.science/paper/IY5M4ZGF"},"agent_actions":{"view_html":"https://pith.science/pith/IY5M4ZGFOEEQFAIHN6DUOOCITS","download_json":"https://pith.science/pith/IY5M4ZGFOEEQFAIHN6DUOOCITS.json","view_paper":"https://pith.science/paper/IY5M4ZGF","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/9909073&json=true","fetch_graph":"https://pith.science/api/pith-number/IY5M4ZGFOEEQFAIHN6DUOOCITS/graph.json","fetch_events":"https://pith.science/api/pith-number/IY5M4ZGFOEEQFAIHN6DUOOCITS/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/IY5M4ZGFOEEQFAIHN6DUOOCITS/action/timestamp_anchor","attest_storage":"https://pith.science/pith/IY5M4ZGFOEEQFAIHN6DUOOCITS/action/storage_attestation","attest_author":"https://pith.science/pith/IY5M4ZGFOEEQFAIHN6DUOOCITS/action/author_attestation","sign_citation":"https://pith.science/pith/IY5M4ZGFOEEQFAIHN6DUOOCITS/action/citation_signature","submit_replication":"https://pith.science/pith/IY5M4ZGFOEEQFAIHN6DUOOCITS/action/replication_record"}},"created_at":"2026-07-04T14:17:05.342376+00:00","updated_at":"2026-07-04T14:17:05.342376+00:00"}