{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2019:XKXLGTPM5TWLFCWJJCMPUJCTAM","short_pith_number":"pith:XKXLGTPM","schema_version":"1.0","canonical_sha256":"baaeb34decececb28ac94898fa24530325e0f223e0bb511631de6a8bfd6c2489","source":{"kind":"arxiv","id":"1902.01344","version":4},"attestation_state":"computed","paper":{"title":"Secular dynamics of binaries in stellar clusters I: general formulation and dependence on cluster potential","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"2) ((1) DAMTP, (2) IAS), Cambridge, Chris Hamilton (1), Roman R. Rafikov (1","submitted_at":"2019-02-04T18:08:22Z","abstract_excerpt":"Orbital evolution of binary systems in dense stellar clusters is important in a variety of contexts: origin of blue stragglers, progenitors of compact object mergers, millisecond pulsars, and so on. Here we consider the general problem of secular evolution of the orbital elements of a binary system driven by the smooth tidal field of an axisymmetric stellar cluster (globular, nuclear, etc.) in which the binary orbits. We derive a secular Hamiltonian (averaged over both the inner Keplerian orbit of the binary and its outer orbit within the cluster) valid to quadrupole order for an arbitrary clu"},"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":"1902.01344","kind":"arxiv","version":4},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.GA","submitted_at":"2019-02-04T18:08:22Z","cross_cats_sorted":[],"title_canon_sha256":"8b78d453f7c5761dbc67b45cedcad4b965d5ef4f4cdbb59a0f9236b20a9d1225","abstract_canon_sha256":"b66317e1c179196f0cc15e376139f8d71b130208be574cb1cda98582326dd587"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T23:57:49.401132Z","signature_b64":"GR9ZqEa+m1K05qwETLvypLXWvID3+NWg1hNDMxkRJab5aaUXEHIdYqhVYgNIkq4U6VPe3YgrmK9gf3pZwj+5Aw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"baaeb34decececb28ac94898fa24530325e0f223e0bb511631de6a8bfd6c2489","last_reissued_at":"2026-07-04T23:57:49.400685Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T23:57:49.400685Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Secular dynamics of binaries in stellar clusters I: general formulation and dependence on cluster potential","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.GA","authors_text":"2) ((1) DAMTP, (2) IAS), Cambridge, Chris Hamilton (1), Roman R. Rafikov (1","submitted_at":"2019-02-04T18:08:22Z","abstract_excerpt":"Orbital evolution of binary systems in dense stellar clusters is important in a variety of contexts: origin of blue stragglers, progenitors of compact object mergers, millisecond pulsars, and so on. Here we consider the general problem of secular evolution of the orbital elements of a binary system driven by the smooth tidal field of an axisymmetric stellar cluster (globular, nuclear, etc.) in which the binary orbits. We derive a secular Hamiltonian (averaged over both the inner Keplerian orbit of the binary and its outer orbit within the cluster) valid to quadrupole order for an arbitrary clu"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1902.01344","kind":"arxiv","version":4},"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/1902.01344/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":"1902.01344","created_at":"2026-07-04T23:57:49.400742+00:00"},{"alias_kind":"arxiv_version","alias_value":"1902.01344v4","created_at":"2026-07-04T23:57:49.400742+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1902.01344","created_at":"2026-07-04T23:57:49.400742+00:00"},{"alias_kind":"pith_short_12","alias_value":"XKXLGTPM5TWL","created_at":"2026-07-04T23:57:49.400742+00:00"},{"alias_kind":"pith_short_16","alias_value":"XKXLGTPM5TWLFCWJ","created_at":"2026-07-04T23:57:49.400742+00:00"},{"alias_kind":"pith_short_8","alias_value":"XKXLGTPM","created_at":"2026-07-04T23:57:49.400742+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2507.11684","citing_title":"The evolution of a supermassive binary black hole in an non-spherical nuclear star cluster","ref_index":43,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/XKXLGTPM5TWLFCWJJCMPUJCTAM","json":"https://pith.science/pith/XKXLGTPM5TWLFCWJJCMPUJCTAM.json","graph_json":"https://pith.science/api/pith-number/XKXLGTPM5TWLFCWJJCMPUJCTAM/graph.json","events_json":"https://pith.science/api/pith-number/XKXLGTPM5TWLFCWJJCMPUJCTAM/events.json","paper":"https://pith.science/paper/XKXLGTPM"},"agent_actions":{"view_html":"https://pith.science/pith/XKXLGTPM5TWLFCWJJCMPUJCTAM","download_json":"https://pith.science/pith/XKXLGTPM5TWLFCWJJCMPUJCTAM.json","view_paper":"https://pith.science/paper/XKXLGTPM","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1902.01344&json=true","fetch_graph":"https://pith.science/api/pith-number/XKXLGTPM5TWLFCWJJCMPUJCTAM/graph.json","fetch_events":"https://pith.science/api/pith-number/XKXLGTPM5TWLFCWJJCMPUJCTAM/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/XKXLGTPM5TWLFCWJJCMPUJCTAM/action/timestamp_anchor","attest_storage":"https://pith.science/pith/XKXLGTPM5TWLFCWJJCMPUJCTAM/action/storage_attestation","attest_author":"https://pith.science/pith/XKXLGTPM5TWLFCWJJCMPUJCTAM/action/author_attestation","sign_citation":"https://pith.science/pith/XKXLGTPM5TWLFCWJJCMPUJCTAM/action/citation_signature","submit_replication":"https://pith.science/pith/XKXLGTPM5TWLFCWJJCMPUJCTAM/action/replication_record"}},"created_at":"2026-07-04T23:57:49.400742+00:00","updated_at":"2026-07-04T23:57:49.400742+00:00"}