{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2003:K5FNAA5HCDLPHJ4AJILRWBECE2","short_pith_number":"pith:K5FNAA5H","schema_version":"1.0","canonical_sha256":"574ad003a710d6f3a7804a171b048226b89a3012be82465b30d670e13d71aa00","source":{"kind":"arxiv","id":"astro-ph/0302296","version":2},"attestation_state":"computed","paper":{"title":"Chaotic Loss Cones, Black Hole Fueling and the M-Sigma Relation","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"David Merritt (Rutgers), M. Y. Poon (Harvard)","submitted_at":"2003-02-14T20:50:15Z","abstract_excerpt":"In classical loss cone theory, stars are supplied to a central black hole via gravitational scattering onto low angular momentum orbits. Higher feeding rates are possible if the gravitational potential near the black hole is non-axisymmetric and the orbits are chaotic. Motivated by recently published, self-consistent models, we evaluate rates of stellar capture and disruption in triaxial nuclei. Rates are found to substantially exceed those in collisionally-resupplied loss cones, as long as an appreciable fraction of the orbits are centrophilic. The mass captured by a black hole after a given "},"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/0302296","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2003-02-14T20:50:15Z","cross_cats_sorted":[],"title_canon_sha256":"0895f2ef9327a875ce23bd65522036e55cec6d93e9c80ee26a5faad4f7178575","abstract_canon_sha256":"9d2e48e1b2ace39853cef40046d1f6b5310aee6e33efde4d980d7ce7374cf4b9"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T16:36:30.231219Z","signature_b64":"NtaNBhUS0PSlRpvPqrm0qOo0+Rr64/TwpvDW6VX5zzXV8aKRvpTDLX6anjfItAabNdlTdEgGscAfdjy+k3A3Aw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"574ad003a710d6f3a7804a171b048226b89a3012be82465b30d670e13d71aa00","last_reissued_at":"2026-07-04T16:36:30.230851Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T16:36:30.230851Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Chaotic Loss Cones, Black Hole Fueling and the M-Sigma Relation","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"David Merritt (Rutgers), M. Y. Poon (Harvard)","submitted_at":"2003-02-14T20:50:15Z","abstract_excerpt":"In classical loss cone theory, stars are supplied to a central black hole via gravitational scattering onto low angular momentum orbits. Higher feeding rates are possible if the gravitational potential near the black hole is non-axisymmetric and the orbits are chaotic. Motivated by recently published, self-consistent models, we evaluate rates of stellar capture and disruption in triaxial nuclei. Rates are found to substantially exceed those in collisionally-resupplied loss cones, as long as an appreciable fraction of the orbits are centrophilic. The mass captured by a black hole after a given "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0302296","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/astro-ph/0302296/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/0302296","created_at":"2026-07-04T16:36:30.230912+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0302296v2","created_at":"2026-07-04T16:36:30.230912+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0302296","created_at":"2026-07-04T16:36:30.230912+00:00"},{"alias_kind":"pith_short_12","alias_value":"K5FNAA5HCDLP","created_at":"2026-07-04T16:36:30.230912+00:00"},{"alias_kind":"pith_short_16","alias_value":"K5FNAA5HCDLPHJ4A","created_at":"2026-07-04T16:36:30.230912+00:00"},{"alias_kind":"pith_short_8","alias_value":"K5FNAA5H","created_at":"2026-07-04T16:36:30.230912+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":23,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/K5FNAA5HCDLPHJ4AJILRWBECE2","json":"https://pith.science/pith/K5FNAA5HCDLPHJ4AJILRWBECE2.json","graph_json":"https://pith.science/api/pith-number/K5FNAA5HCDLPHJ4AJILRWBECE2/graph.json","events_json":"https://pith.science/api/pith-number/K5FNAA5HCDLPHJ4AJILRWBECE2/events.json","paper":"https://pith.science/paper/K5FNAA5H"},"agent_actions":{"view_html":"https://pith.science/pith/K5FNAA5HCDLPHJ4AJILRWBECE2","download_json":"https://pith.science/pith/K5FNAA5HCDLPHJ4AJILRWBECE2.json","view_paper":"https://pith.science/paper/K5FNAA5H","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0302296&json=true","fetch_graph":"https://pith.science/api/pith-number/K5FNAA5HCDLPHJ4AJILRWBECE2/graph.json","fetch_events":"https://pith.science/api/pith-number/K5FNAA5HCDLPHJ4AJILRWBECE2/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/K5FNAA5HCDLPHJ4AJILRWBECE2/action/timestamp_anchor","attest_storage":"https://pith.science/pith/K5FNAA5HCDLPHJ4AJILRWBECE2/action/storage_attestation","attest_author":"https://pith.science/pith/K5FNAA5HCDLPHJ4AJILRWBECE2/action/author_attestation","sign_citation":"https://pith.science/pith/K5FNAA5HCDLPHJ4AJILRWBECE2/action/citation_signature","submit_replication":"https://pith.science/pith/K5FNAA5HCDLPHJ4AJILRWBECE2/action/replication_record"}},"created_at":"2026-07-04T16:36:30.230912+00:00","updated_at":"2026-07-04T16:36:30.230912+00:00"}