{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:WEE3IYMRDPNHDLYA2JZ4PP3ZWJ","short_pith_number":"pith:WEE3IYMR","schema_version":"1.0","canonical_sha256":"b109b461911bda71af00d273c7bf79b263e1d024fae355c97e62e03d0ac0375b","source":{"kind":"arxiv","id":"2209.03982","version":1},"attestation_state":"computed","paper":{"title":"A simple and accurate prescription for the tidal disruption radius of a star and the peak accretion rate in tidal disruption events","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA","astro-ph.SR"],"primary_cat":"astro-ph.HE","authors_text":"Chris Nixon, Eric R. Coughlin","submitted_at":"2022-09-08T18:01:09Z","abstract_excerpt":"A star destroyed by a supermassive black hole (SMBH) in a tidal disruption event (TDE) enables the study of SMBHs. We propose that the distance within which a star is completely destroyed by a SMBH, defined $r_{\\rm t, c}$, is accurately estimated by equating the SMBH tidal field (including numerical factors) to the maximum gravitational field in the star. We demonstrate that this definition accurately reproduces the critical $\\beta_{\\rm c} = r_{\\rm t}/r_{\\rm t, c}$, where $r_{\\rm t} = R_{\\star}\\left(M_{\\bullet}/M_{\\star}\\right)^{1/3}$ is the standard tidal radius with $R_{\\star}$ and $M_{\\star"},"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":"2209.03982","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2022-09-08T18:01:09Z","cross_cats_sorted":["astro-ph.GA","astro-ph.SR"],"title_canon_sha256":"e1787e194aa775db776d3b9efa801dbeeafe7d9c3ccfb3694b5750f40e6e1054","abstract_canon_sha256":"d3ebfe5d652f0cba827bf48af5f7ae2320f242eec3757fcbeeb0fe5cdd71cbd6"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T04:59:32.778149Z","signature_b64":"+SAN9q0pxNTP1zrR285NBFiqormG1oSF7Z6EcrCnQ8a0ZzntRUfhCfieoBpueb9E3ST9kJEfmOmN2YSdus1VBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"b109b461911bda71af00d273c7bf79b263e1d024fae355c97e62e03d0ac0375b","last_reissued_at":"2026-07-05T04:59:32.777758Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T04:59:32.777758Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"A simple and accurate prescription for the tidal disruption radius of a star and the peak accretion rate in tidal disruption events","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.GA","astro-ph.SR"],"primary_cat":"astro-ph.HE","authors_text":"Chris Nixon, Eric R. Coughlin","submitted_at":"2022-09-08T18:01:09Z","abstract_excerpt":"A star destroyed by a supermassive black hole (SMBH) in a tidal disruption event (TDE) enables the study of SMBHs. We propose that the distance within which a star is completely destroyed by a SMBH, defined $r_{\\rm t, c}$, is accurately estimated by equating the SMBH tidal field (including numerical factors) to the maximum gravitational field in the star. We demonstrate that this definition accurately reproduces the critical $\\beta_{\\rm c} = r_{\\rm t}/r_{\\rm t, c}$, where $r_{\\rm t} = R_{\\star}\\left(M_{\\bullet}/M_{\\star}\\right)^{1/3}$ is the standard tidal radius with $R_{\\star}$ and $M_{\\star"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2209.03982","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/2209.03982/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":"2209.03982","created_at":"2026-07-05T04:59:32.777813+00:00"},{"alias_kind":"arxiv_version","alias_value":"2209.03982v1","created_at":"2026-07-05T04:59:32.777813+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2209.03982","created_at":"2026-07-05T04:59:32.777813+00:00"},{"alias_kind":"pith_short_12","alias_value":"WEE3IYMRDPNH","created_at":"2026-07-05T04:59:32.777813+00:00"},{"alias_kind":"pith_short_16","alias_value":"WEE3IYMRDPNHDLYA","created_at":"2026-07-05T04:59:32.777813+00:00"},{"alias_kind":"pith_short_8","alias_value":"WEE3IYMR","created_at":"2026-07-05T04:59:32.777813+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2412.15938","citing_title":"Chaotic orbital dynamics of pulsating stars around black holes surrounded by dark matter halos","ref_index":94,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/WEE3IYMRDPNHDLYA2JZ4PP3ZWJ","json":"https://pith.science/pith/WEE3IYMRDPNHDLYA2JZ4PP3ZWJ.json","graph_json":"https://pith.science/api/pith-number/WEE3IYMRDPNHDLYA2JZ4PP3ZWJ/graph.json","events_json":"https://pith.science/api/pith-number/WEE3IYMRDPNHDLYA2JZ4PP3ZWJ/events.json","paper":"https://pith.science/paper/WEE3IYMR"},"agent_actions":{"view_html":"https://pith.science/pith/WEE3IYMRDPNHDLYA2JZ4PP3ZWJ","download_json":"https://pith.science/pith/WEE3IYMRDPNHDLYA2JZ4PP3ZWJ.json","view_paper":"https://pith.science/paper/WEE3IYMR","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2209.03982&json=true","fetch_graph":"https://pith.science/api/pith-number/WEE3IYMRDPNHDLYA2JZ4PP3ZWJ/graph.json","fetch_events":"https://pith.science/api/pith-number/WEE3IYMRDPNHDLYA2JZ4PP3ZWJ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/WEE3IYMRDPNHDLYA2JZ4PP3ZWJ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/WEE3IYMRDPNHDLYA2JZ4PP3ZWJ/action/storage_attestation","attest_author":"https://pith.science/pith/WEE3IYMRDPNHDLYA2JZ4PP3ZWJ/action/author_attestation","sign_citation":"https://pith.science/pith/WEE3IYMRDPNHDLYA2JZ4PP3ZWJ/action/citation_signature","submit_replication":"https://pith.science/pith/WEE3IYMRDPNHDLYA2JZ4PP3ZWJ/action/replication_record"}},"created_at":"2026-07-05T04:59:32.777813+00:00","updated_at":"2026-07-05T04:59:32.777813+00:00"}