{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:N6SYDG6LA23TMTH3JZTBWF77IH","short_pith_number":"pith:N6SYDG6L","schema_version":"1.0","canonical_sha256":"6fa5819bcb06b7364cfb4e661b17ff41f83ba92fd7b3029548574136b64399f8","source":{"kind":"arxiv","id":"2505.13951","version":1},"attestation_state":"computed","paper":{"title":"Accretion of AGN Stars under Influence of Disk Geometry","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.HE","authors_text":"Jeremy Goodman, Yan-Fei Jiang, Yi-Xian Chen","submitted_at":"2025-05-20T05:29:26Z","abstract_excerpt":"Massive stars can form within or be captured by AGN disks, influencing both the thermal structure and metallicity of the disk environment. In a previous work, we investigated isotropic accretion onto massive stars from a gas-rich, high-entropy background. Here, we consider a more realistic scenario by incorporating the stratified geometry of the background disk in our 3D radiation hydrodynamic simulatons. We find that accretion remains relatively isotropic when the disk is hot enough and the scale height is thicker than the accretion flow's nominal supersonic critical radius $R{crit}$ (sub-the"},"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":"2505.13951","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.HE","submitted_at":"2025-05-20T05:29:26Z","cross_cats_sorted":["astro-ph.SR"],"title_canon_sha256":"83880a60d2177f58c6eaaad8e4924b71f99f07f9940d45db6a45eafdb006e030","abstract_canon_sha256":"04796ff2ea297b47c08827ba41d3b34514ec7b2c2fc3b5e054a33d3fe07bb49f"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T11:05:53.565616Z","signature_b64":"VpeLaxiznAR59GDiP1mPBalVFPTt63GlbmsXJ9QUpM1CGYFaaQnLXc4d4z7VtqvsdPaVrEYJDZbjYJ7ZMC39BA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"6fa5819bcb06b7364cfb4e661b17ff41f83ba92fd7b3029548574136b64399f8","last_reissued_at":"2026-07-05T11:05:53.565114Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T11:05:53.565114Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Accretion of AGN Stars under Influence of Disk Geometry","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.HE","authors_text":"Jeremy Goodman, Yan-Fei Jiang, Yi-Xian Chen","submitted_at":"2025-05-20T05:29:26Z","abstract_excerpt":"Massive stars can form within or be captured by AGN disks, influencing both the thermal structure and metallicity of the disk environment. In a previous work, we investigated isotropic accretion onto massive stars from a gas-rich, high-entropy background. Here, we consider a more realistic scenario by incorporating the stratified geometry of the background disk in our 3D radiation hydrodynamic simulatons. We find that accretion remains relatively isotropic when the disk is hot enough and the scale height is thicker than the accretion flow's nominal supersonic critical radius $R{crit}$ (sub-the"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2505.13951","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/2505.13951/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":"2505.13951","created_at":"2026-07-05T11:05:53.565170+00:00"},{"alias_kind":"arxiv_version","alias_value":"2505.13951v1","created_at":"2026-07-05T11:05:53.565170+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2505.13951","created_at":"2026-07-05T11:05:53.565170+00:00"},{"alias_kind":"pith_short_12","alias_value":"N6SYDG6LA23T","created_at":"2026-07-05T11:05:53.565170+00:00"},{"alias_kind":"pith_short_16","alias_value":"N6SYDG6LA23TMTH3","created_at":"2026-07-05T11:05:53.565170+00:00"},{"alias_kind":"pith_short_8","alias_value":"N6SYDG6L","created_at":"2026-07-05T11:05:53.565170+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2506.08801","citing_title":"Using gravitational waves and multi-messenger Astronomy to reverse-engineer the properties of galactic nuclei","ref_index":33,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/N6SYDG6LA23TMTH3JZTBWF77IH","json":"https://pith.science/pith/N6SYDG6LA23TMTH3JZTBWF77IH.json","graph_json":"https://pith.science/api/pith-number/N6SYDG6LA23TMTH3JZTBWF77IH/graph.json","events_json":"https://pith.science/api/pith-number/N6SYDG6LA23TMTH3JZTBWF77IH/events.json","paper":"https://pith.science/paper/N6SYDG6L"},"agent_actions":{"view_html":"https://pith.science/pith/N6SYDG6LA23TMTH3JZTBWF77IH","download_json":"https://pith.science/pith/N6SYDG6LA23TMTH3JZTBWF77IH.json","view_paper":"https://pith.science/paper/N6SYDG6L","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2505.13951&json=true","fetch_graph":"https://pith.science/api/pith-number/N6SYDG6LA23TMTH3JZTBWF77IH/graph.json","fetch_events":"https://pith.science/api/pith-number/N6SYDG6LA23TMTH3JZTBWF77IH/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/N6SYDG6LA23TMTH3JZTBWF77IH/action/timestamp_anchor","attest_storage":"https://pith.science/pith/N6SYDG6LA23TMTH3JZTBWF77IH/action/storage_attestation","attest_author":"https://pith.science/pith/N6SYDG6LA23TMTH3JZTBWF77IH/action/author_attestation","sign_citation":"https://pith.science/pith/N6SYDG6LA23TMTH3JZTBWF77IH/action/citation_signature","submit_replication":"https://pith.science/pith/N6SYDG6LA23TMTH3JZTBWF77IH/action/replication_record"}},"created_at":"2026-07-05T11:05:53.565170+00:00","updated_at":"2026-07-05T11:05:53.565170+00:00"}