{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:UQL572F3JJTLHUT2IGJ5BHYXPQ","short_pith_number":"pith:UQL572F3","schema_version":"1.0","canonical_sha256":"a417dfe8bb4a66b3d27a4193d09f177c2dfae0390c77a5d60d1de125096eb7e2","source":{"kind":"arxiv","id":"2410.04961","version":1},"attestation_state":"computed","paper":{"title":"Changing-Look Inspirals: Trends and Switches in AGN Disk Emission as Signposts for Merging Black Hole Binaries","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Jonathan Zrake, Madeline Clyburn, Samuel Feyan","submitted_at":"2024-10-07T12:00:17Z","abstract_excerpt":"Using grid-based hydrodynamics simulations and analytic modeling, we compute the electromagnetic (EM) signatures of gravitational wave (GW) driven inspirals of massive black hole binaries that accrete gas from circumbinary disks, exploring the effects of varying gas temperatures, viscosity laws, and binary mass ratios. Our main finding is that active galactic nuclei (AGN's) that host inspiraling binaries can exhibit two sub-types of long-term secular variability patterns: Type-A events which dim before merger and brighten afterward, and Type-B events which brighten before merger and dim afterw"},"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":"2410.04961","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2024-10-07T12:00:17Z","cross_cats_sorted":[],"title_canon_sha256":"66750e17bd18a8b3983c8b95c282af92042eecc886692a6e6907b673c60bc0bd","abstract_canon_sha256":"302decc190b7515b122f5fb432b375782dd04e60c97c4f74e8069b18fd4030fa"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T10:19:29.259026Z","signature_b64":"tFYjn5VDiFns1vtVFQgtTZqb0v2eZqFGHv3tq098nc3wnBDcKB9a554rBnFNDVxJn6Qz1vPunoulwT0xvkdxCQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"a417dfe8bb4a66b3d27a4193d09f177c2dfae0390c77a5d60d1de125096eb7e2","last_reissued_at":"2026-07-05T10:19:29.258538Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T10:19:29.258538Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Changing-Look Inspirals: Trends and Switches in AGN Disk Emission as Signposts for Merging Black Hole Binaries","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Jonathan Zrake, Madeline Clyburn, Samuel Feyan","submitted_at":"2024-10-07T12:00:17Z","abstract_excerpt":"Using grid-based hydrodynamics simulations and analytic modeling, we compute the electromagnetic (EM) signatures of gravitational wave (GW) driven inspirals of massive black hole binaries that accrete gas from circumbinary disks, exploring the effects of varying gas temperatures, viscosity laws, and binary mass ratios. Our main finding is that active galactic nuclei (AGN's) that host inspiraling binaries can exhibit two sub-types of long-term secular variability patterns: Type-A events which dim before merger and brighten afterward, and Type-B events which brighten before merger and dim afterw"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2410.04961","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/2410.04961/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":"2410.04961","created_at":"2026-07-05T10:19:29.258596+00:00"},{"alias_kind":"arxiv_version","alias_value":"2410.04961v1","created_at":"2026-07-05T10:19:29.258596+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2410.04961","created_at":"2026-07-05T10:19:29.258596+00:00"},{"alias_kind":"pith_short_12","alias_value":"UQL572F3JJTL","created_at":"2026-07-05T10:19:29.258596+00:00"},{"alias_kind":"pith_short_16","alias_value":"UQL572F3JJTLHUT2","created_at":"2026-07-05T10:19:29.258596+00:00"},{"alias_kind":"pith_short_8","alias_value":"UQL572F3","created_at":"2026-07-05T10:19:29.258596+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":20,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/UQL572F3JJTLHUT2IGJ5BHYXPQ","json":"https://pith.science/pith/UQL572F3JJTLHUT2IGJ5BHYXPQ.json","graph_json":"https://pith.science/api/pith-number/UQL572F3JJTLHUT2IGJ5BHYXPQ/graph.json","events_json":"https://pith.science/api/pith-number/UQL572F3JJTLHUT2IGJ5BHYXPQ/events.json","paper":"https://pith.science/paper/UQL572F3"},"agent_actions":{"view_html":"https://pith.science/pith/UQL572F3JJTLHUT2IGJ5BHYXPQ","download_json":"https://pith.science/pith/UQL572F3JJTLHUT2IGJ5BHYXPQ.json","view_paper":"https://pith.science/paper/UQL572F3","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2410.04961&json=true","fetch_graph":"https://pith.science/api/pith-number/UQL572F3JJTLHUT2IGJ5BHYXPQ/graph.json","fetch_events":"https://pith.science/api/pith-number/UQL572F3JJTLHUT2IGJ5BHYXPQ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/UQL572F3JJTLHUT2IGJ5BHYXPQ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/UQL572F3JJTLHUT2IGJ5BHYXPQ/action/storage_attestation","attest_author":"https://pith.science/pith/UQL572F3JJTLHUT2IGJ5BHYXPQ/action/author_attestation","sign_citation":"https://pith.science/pith/UQL572F3JJTLHUT2IGJ5BHYXPQ/action/citation_signature","submit_replication":"https://pith.science/pith/UQL572F3JJTLHUT2IGJ5BHYXPQ/action/replication_record"}},"created_at":"2026-07-05T10:19:29.258596+00:00","updated_at":"2026-07-05T10:19:29.258596+00:00"}