{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:1996:TMV2LVULYMRB47YWKSOCAFASSL","short_pith_number":"pith:TMV2LVUL","schema_version":"1.0","canonical_sha256":"9b2ba5d68bc3221e7f16549c20141292dab4a0836fe856a166d1fe61a280f251","source":{"kind":"arxiv","id":"astro-ph/9601106","version":2},"attestation_state":"computed","paper":{"title":"Line Emission from an Accretion Disk around a Rotating Black Hole: Toward a Measurement of Frame Dragging","license":"","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph","authors_text":"Benjamin C. Bromley, Kaiyou Chen, Warner A. Miller","submitted_at":"1996-01-19T23:11:38Z","abstract_excerpt":"Line emission from an accretion disk and a corotating hot spot about a rotating black hole are considered for possible signatures of the frame-dragging effect. We explicitly compare integrated line profiles from a geometrically thin disk about a Schwarzschild and an extreme Kerr black hole, and show that the line profile differences are small if the inner radius of the disk is near or above the Schwarzschild stable-orbit limit of radius 6GM/c^2. However, if the inner disk radius extends below this limit, as is possible in the extreme Kerr spacetime, then differences can become significant, esp"},"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/9601106","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"1996-01-19T23:11:38Z","cross_cats_sorted":["gr-qc"],"title_canon_sha256":"7d33e96cafc5c92db95c6ccab6151b6f7682854cbf684ef9672b6fe015019f3c","abstract_canon_sha256":"6945acdc773dc9af5d79280c73890666cfb2f3dc9ec702a3a7c2161c369963e0"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T15:59:33.705360Z","signature_b64":"BJQU5pvT24vM86NKifc9hdaN9HTErwwrQi+hMDCY13KqzprF3tzCtHfH7eELefF3QlJJpi3sS8DqtR9TmHDICg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"9b2ba5d68bc3221e7f16549c20141292dab4a0836fe856a166d1fe61a280f251","last_reissued_at":"2026-07-04T15:59:33.704789Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T15:59:33.704789Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Line Emission from an Accretion Disk around a Rotating Black Hole: Toward a Measurement of Frame Dragging","license":"","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph","authors_text":"Benjamin C. Bromley, Kaiyou Chen, Warner A. Miller","submitted_at":"1996-01-19T23:11:38Z","abstract_excerpt":"Line emission from an accretion disk and a corotating hot spot about a rotating black hole are considered for possible signatures of the frame-dragging effect. We explicitly compare integrated line profiles from a geometrically thin disk about a Schwarzschild and an extreme Kerr black hole, and show that the line profile differences are small if the inner radius of the disk is near or above the Schwarzschild stable-orbit limit of radius 6GM/c^2. However, if the inner disk radius extends below this limit, as is possible in the extreme Kerr spacetime, then differences can become significant, esp"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/9601106","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/9601106/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/9601106","created_at":"2026-07-04T15:59:33.704858+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/9601106v2","created_at":"2026-07-04T15:59:33.704858+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/9601106","created_at":"2026-07-04T15:59:33.704858+00:00"},{"alias_kind":"pith_short_12","alias_value":"TMV2LVULYMRB","created_at":"2026-07-04T15:59:33.704858+00:00"},{"alias_kind":"pith_short_16","alias_value":"TMV2LVULYMRB47YW","created_at":"2026-07-04T15:59:33.704858+00:00"},{"alias_kind":"pith_short_8","alias_value":"TMV2LVUL","created_at":"2026-07-04T15:59:33.704858+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2504.12072","citing_title":"Observational properties of regular black holes in Asymptotic Safety","ref_index":82,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/TMV2LVULYMRB47YWKSOCAFASSL","json":"https://pith.science/pith/TMV2LVULYMRB47YWKSOCAFASSL.json","graph_json":"https://pith.science/api/pith-number/TMV2LVULYMRB47YWKSOCAFASSL/graph.json","events_json":"https://pith.science/api/pith-number/TMV2LVULYMRB47YWKSOCAFASSL/events.json","paper":"https://pith.science/paper/TMV2LVUL"},"agent_actions":{"view_html":"https://pith.science/pith/TMV2LVULYMRB47YWKSOCAFASSL","download_json":"https://pith.science/pith/TMV2LVULYMRB47YWKSOCAFASSL.json","view_paper":"https://pith.science/paper/TMV2LVUL","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/9601106&json=true","fetch_graph":"https://pith.science/api/pith-number/TMV2LVULYMRB47YWKSOCAFASSL/graph.json","fetch_events":"https://pith.science/api/pith-number/TMV2LVULYMRB47YWKSOCAFASSL/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/TMV2LVULYMRB47YWKSOCAFASSL/action/timestamp_anchor","attest_storage":"https://pith.science/pith/TMV2LVULYMRB47YWKSOCAFASSL/action/storage_attestation","attest_author":"https://pith.science/pith/TMV2LVULYMRB47YWKSOCAFASSL/action/author_attestation","sign_citation":"https://pith.science/pith/TMV2LVULYMRB47YWKSOCAFASSL/action/citation_signature","submit_replication":"https://pith.science/pith/TMV2LVULYMRB47YWKSOCAFASSL/action/replication_record"}},"created_at":"2026-07-04T15:59:33.704858+00:00","updated_at":"2026-07-04T15:59:33.704858+00:00"}