{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2023:3DTTQIAYIZBT2WS23TLH2APTH3","short_pith_number":"pith:3DTTQIAY","schema_version":"1.0","canonical_sha256":"d8e738201846433d5a5adcd67d01f33ec83a6ba49cf3f5a854dd74e8dd5323a8","source":{"kind":"arxiv","id":"2309.06028","version":2},"attestation_state":"computed","paper":{"title":"Viscous torque in turbulent magnetized AGN accretion disks and its effects on EMRI's gravitational waves","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.GA","gr-qc"],"primary_cat":"astro-ph.HE","authors_text":"Agnieszka Janiuk, Fatemeh Hossein Nouri","submitted_at":"2023-09-12T07:59:41Z","abstract_excerpt":"The merger of supermassive black holes (SMBHs) produces mHz gravitational waves (GW), which are potentially detectable by future Laser Interferometer Space Antenna (LISA). Such binary systems are usually embedded in an accretion disk environment at the centre of the active galactic nucleus (AGN). Recent studies suggest the plasma environment imposes measurable imprints on the GW signal if the mass ratio of the binary is around q $ \\sim10^{-4}-10^{-3}$. The effect of the gaseous environment on the GW signal is strongly dependent on the disk's parameters, therefore it is believed that future low"},"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":"2309.06028","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.HE","submitted_at":"2023-09-12T07:59:41Z","cross_cats_sorted":["astro-ph.GA","gr-qc"],"title_canon_sha256":"d6416dfab6dae884582ba6d6b10921f7d0436bce0b2eff2f3e8fd01b2c8d1005","abstract_canon_sha256":"938c7fd7d0774980136d9582ef65b3e70f09bd5c2e5cdd2d6951b40a359f81b9"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T08:44:34.275419Z","signature_b64":"TbZ5g9KlCEe3bwsQ2XGnvfQ0+MqKH9Y/ZuuTahHMBlo6FEMR6JpleV+Fv/RAgoNvQYUgjw3fpTVZDn6VfyAMDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d8e738201846433d5a5adcd67d01f33ec83a6ba49cf3f5a854dd74e8dd5323a8","last_reissued_at":"2026-07-05T08:44:34.274983Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T08:44:34.274983Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Viscous torque in turbulent magnetized AGN accretion disks and its effects on EMRI's gravitational waves","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.GA","gr-qc"],"primary_cat":"astro-ph.HE","authors_text":"Agnieszka Janiuk, Fatemeh Hossein Nouri","submitted_at":"2023-09-12T07:59:41Z","abstract_excerpt":"The merger of supermassive black holes (SMBHs) produces mHz gravitational waves (GW), which are potentially detectable by future Laser Interferometer Space Antenna (LISA). Such binary systems are usually embedded in an accretion disk environment at the centre of the active galactic nucleus (AGN). Recent studies suggest the plasma environment imposes measurable imprints on the GW signal if the mass ratio of the binary is around q $ \\sim10^{-4}-10^{-3}$. The effect of the gaseous environment on the GW signal is strongly dependent on the disk's parameters, therefore it is believed that future low"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2309.06028","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/2309.06028/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":"2309.06028","created_at":"2026-07-05T08:44:34.275042+00:00"},{"alias_kind":"arxiv_version","alias_value":"2309.06028v2","created_at":"2026-07-05T08:44:34.275042+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2309.06028","created_at":"2026-07-05T08:44:34.275042+00:00"},{"alias_kind":"pith_short_12","alias_value":"3DTTQIAYIZBT","created_at":"2026-07-05T08:44:34.275042+00:00"},{"alias_kind":"pith_short_16","alias_value":"3DTTQIAYIZBT2WS2","created_at":"2026-07-05T08:44:34.275042+00:00"},{"alias_kind":"pith_short_8","alias_value":"3DTTQIAY","created_at":"2026-07-05T08:44:34.275042+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.10942","citing_title":"Probing Active Galactic Nuclei and Measuring the Hubble constant with Extreme-Mass-Ratio Inspirals","ref_index":24,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/3DTTQIAYIZBT2WS23TLH2APTH3","json":"https://pith.science/pith/3DTTQIAYIZBT2WS23TLH2APTH3.json","graph_json":"https://pith.science/api/pith-number/3DTTQIAYIZBT2WS23TLH2APTH3/graph.json","events_json":"https://pith.science/api/pith-number/3DTTQIAYIZBT2WS23TLH2APTH3/events.json","paper":"https://pith.science/paper/3DTTQIAY"},"agent_actions":{"view_html":"https://pith.science/pith/3DTTQIAYIZBT2WS23TLH2APTH3","download_json":"https://pith.science/pith/3DTTQIAYIZBT2WS23TLH2APTH3.json","view_paper":"https://pith.science/paper/3DTTQIAY","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2309.06028&json=true","fetch_graph":"https://pith.science/api/pith-number/3DTTQIAYIZBT2WS23TLH2APTH3/graph.json","fetch_events":"https://pith.science/api/pith-number/3DTTQIAYIZBT2WS23TLH2APTH3/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/3DTTQIAYIZBT2WS23TLH2APTH3/action/timestamp_anchor","attest_storage":"https://pith.science/pith/3DTTQIAYIZBT2WS23TLH2APTH3/action/storage_attestation","attest_author":"https://pith.science/pith/3DTTQIAYIZBT2WS23TLH2APTH3/action/author_attestation","sign_citation":"https://pith.science/pith/3DTTQIAYIZBT2WS23TLH2APTH3/action/citation_signature","submit_replication":"https://pith.science/pith/3DTTQIAYIZBT2WS23TLH2APTH3/action/replication_record"}},"created_at":"2026-07-05T08:44:34.275042+00:00","updated_at":"2026-07-05T08:44:34.275042+00:00"}