{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2007:FIIY6EEO77RP44N5ZU6DHZEOQE","short_pith_number":"pith:FIIY6EEO","schema_version":"1.0","canonical_sha256":"2a118f108effe2fe71bdcd3c33e48e813417ce0851ae20ea9058a2e54ea03f2a","source":{"kind":"arxiv","id":"astro-ph/0701778","version":1},"attestation_state":"computed","paper":{"title":"Simulating the Emission and Outflows from Accretion Disks","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Charles F. Gammie, Laura G. Book, Po Kin Leung, Scott C. Noble","submitted_at":"2007-01-26T19:30:37Z","abstract_excerpt":"The radio source Sagittarius A* (Sgr A*) is believed to be a hot, inhomogeneous, magnetized plasma flowing near the event horizon of the 3 million solar mass black hole at the galactic center. At a distance of 8000 parsecs the black hole would be among the largest black holes as judged by angular size. Recent observations are consistent with the idea that the millimeter and sub-millimeter photons are dominated by optically thin, thermal synchrotron emission. Anticipating future Very Long Baseline Interferometry (VLBI) observations of Sgr A* at these wavelengths, we present here the first dynam"},"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/0701778","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2007-01-26T19:30:37Z","cross_cats_sorted":[],"title_canon_sha256":"4ea075a9ab890d9a5db54bf58ec507e104409568e0dd8d3c50e2c7be1be23309","abstract_canon_sha256":"bdf3a22505df5b8927be305711c0cc42d840c6e73f30088aa15bc5b66d8aa43c"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T15:18:47.036093Z","signature_b64":"8R0qPuFrVB/dWvlr0OUvoDcxnQfrnYys4776Wdotrm2fq1WUFHrIOOixDDrvt9Tt2HgHvwj+duWBbJeX/rSvBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"2a118f108effe2fe71bdcd3c33e48e813417ce0851ae20ea9058a2e54ea03f2a","last_reissued_at":"2026-07-04T15:18:47.035677Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T15:18:47.035677Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Simulating the Emission and Outflows from Accretion Disks","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Charles F. Gammie, Laura G. Book, Po Kin Leung, Scott C. Noble","submitted_at":"2007-01-26T19:30:37Z","abstract_excerpt":"The radio source Sagittarius A* (Sgr A*) is believed to be a hot, inhomogeneous, magnetized plasma flowing near the event horizon of the 3 million solar mass black hole at the galactic center. At a distance of 8000 parsecs the black hole would be among the largest black holes as judged by angular size. Recent observations are consistent with the idea that the millimeter and sub-millimeter photons are dominated by optically thin, thermal synchrotron emission. Anticipating future Very Long Baseline Interferometry (VLBI) observations of Sgr A* at these wavelengths, we present here the first dynam"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0701778","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/astro-ph/0701778/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/0701778","created_at":"2026-07-04T15:18:47.035740+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0701778v1","created_at":"2026-07-04T15:18:47.035740+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0701778","created_at":"2026-07-04T15:18:47.035740+00:00"},{"alias_kind":"pith_short_12","alias_value":"FIIY6EEO77RP","created_at":"2026-07-04T15:18:47.035740+00:00"},{"alias_kind":"pith_short_16","alias_value":"FIIY6EEO77RP44N5","created_at":"2026-07-04T15:18:47.035740+00:00"},{"alias_kind":"pith_short_8","alias_value":"FIIY6EEO","created_at":"2026-07-04T15:18:47.035740+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":3,"sample":[{"citing_arxiv_id":"2606.26166","citing_title":"Images of Braneworld black holes with radiatively inefficient accretion flows","ref_index":40,"is_internal_anchor":true},{"citing_arxiv_id":"2606.19320","citing_title":"GRMHD and GRRT Simulations of Black Hole Accretion: Flares, Precession, and Complex Spacetimes","ref_index":279,"is_internal_anchor":true},{"citing_arxiv_id":"2507.03857","citing_title":"Bright ring features and polarization structures in Kerr-Sen black hole images illuminated by radiatively inefficient accretion flows","ref_index":44,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/FIIY6EEO77RP44N5ZU6DHZEOQE","json":"https://pith.science/pith/FIIY6EEO77RP44N5ZU6DHZEOQE.json","graph_json":"https://pith.science/api/pith-number/FIIY6EEO77RP44N5ZU6DHZEOQE/graph.json","events_json":"https://pith.science/api/pith-number/FIIY6EEO77RP44N5ZU6DHZEOQE/events.json","paper":"https://pith.science/paper/FIIY6EEO"},"agent_actions":{"view_html":"https://pith.science/pith/FIIY6EEO77RP44N5ZU6DHZEOQE","download_json":"https://pith.science/pith/FIIY6EEO77RP44N5ZU6DHZEOQE.json","view_paper":"https://pith.science/paper/FIIY6EEO","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0701778&json=true","fetch_graph":"https://pith.science/api/pith-number/FIIY6EEO77RP44N5ZU6DHZEOQE/graph.json","fetch_events":"https://pith.science/api/pith-number/FIIY6EEO77RP44N5ZU6DHZEOQE/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/FIIY6EEO77RP44N5ZU6DHZEOQE/action/timestamp_anchor","attest_storage":"https://pith.science/pith/FIIY6EEO77RP44N5ZU6DHZEOQE/action/storage_attestation","attest_author":"https://pith.science/pith/FIIY6EEO77RP44N5ZU6DHZEOQE/action/author_attestation","sign_citation":"https://pith.science/pith/FIIY6EEO77RP44N5ZU6DHZEOQE/action/citation_signature","submit_replication":"https://pith.science/pith/FIIY6EEO77RP44N5ZU6DHZEOQE/action/replication_record"}},"created_at":"2026-07-04T15:18:47.035740+00:00","updated_at":"2026-07-04T15:18:47.035740+00:00"}