{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:24B3PAQW2ZSABNHTZ2EXOCJXZA","short_pith_number":"pith:24B3PAQW","schema_version":"1.0","canonical_sha256":"d703b78216d66400b4f3ce89770937c81586672f347465fed3217b33e28f7ccb","source":{"kind":"arxiv","id":"2108.12380","version":2},"attestation_state":"computed","paper":{"title":"Jets in Magnetically Arrested Hot Accretion Flows: Geometry, Power and Black Hole Spindown","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Andrew Chael, Angelo Ricarte, Brandon Curd, Koushik Chatterjee, Ramesh Narayan","submitted_at":"2021-08-27T16:31:56Z","abstract_excerpt":"We present the results of nine simulations of radiatively-inefficient magnetically arrested disks (MADs) across different values of the black hole spin parameter $a_*$: $-0.9$, $-0.7$, $-0.5$, $-0.3$, 0, 0.3, 0.5, 0.7, and 0.9. Each simulation was run up to $t \\gtrsim 100,000\\,GM/c^3$ to ensure disk inflow equilibrium out to large radii. We find that the saturated magnetic flux level, and consequently also jet power, of MAD disks depends strongly on the black hole spin, confirming previous results. Prograde disks saturate at a much higher relative magnetic flux and have more powerful jets than"},"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":"2108.12380","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.HE","submitted_at":"2021-08-27T16:31:56Z","cross_cats_sorted":[],"title_canon_sha256":"8017a05fc740ff178d01e40fea9bb81201b1e3dde10af631c64d53e25c6163ae","abstract_canon_sha256":"d7c7bf5db9042396a651690a1647d9f8187e3104e9e23ef85e5727f4d611c1b4"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T03:57:11.373391Z","signature_b64":"h73nF90zHQfgugO6RmM6AjBLBdwWqSHHpH3M99gkxbxOEE8oMBhC+sewBOl7gkI4B9KipIUOgGCnvYYNy4cbAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d703b78216d66400b4f3ce89770937c81586672f347465fed3217b33e28f7ccb","last_reissued_at":"2026-07-05T03:57:11.372891Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T03:57:11.372891Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Jets in Magnetically Arrested Hot Accretion Flows: Geometry, Power and Black Hole Spindown","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Andrew Chael, Angelo Ricarte, Brandon Curd, Koushik Chatterjee, Ramesh Narayan","submitted_at":"2021-08-27T16:31:56Z","abstract_excerpt":"We present the results of nine simulations of radiatively-inefficient magnetically arrested disks (MADs) across different values of the black hole spin parameter $a_*$: $-0.9$, $-0.7$, $-0.5$, $-0.3$, 0, 0.3, 0.5, 0.7, and 0.9. Each simulation was run up to $t \\gtrsim 100,000\\,GM/c^3$ to ensure disk inflow equilibrium out to large radii. We find that the saturated magnetic flux level, and consequently also jet power, of MAD disks depends strongly on the black hole spin, confirming previous results. Prograde disks saturate at a much higher relative magnetic flux and have more powerful jets than"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2108.12380","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/2108.12380/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":"2108.12380","created_at":"2026-07-05T03:57:11.372950+00:00"},{"alias_kind":"arxiv_version","alias_value":"2108.12380v2","created_at":"2026-07-05T03:57:11.372950+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2108.12380","created_at":"2026-07-05T03:57:11.372950+00:00"},{"alias_kind":"pith_short_12","alias_value":"24B3PAQW2ZSA","created_at":"2026-07-05T03:57:11.372950+00:00"},{"alias_kind":"pith_short_16","alias_value":"24B3PAQW2ZSABNHT","created_at":"2026-07-05T03:57:11.372950+00:00"},{"alias_kind":"pith_short_8","alias_value":"24B3PAQW","created_at":"2026-07-05T03:57:11.372950+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2604.09046","citing_title":"Relative Magnification Factor of Point Sources on Accretion Disks","ref_index":22,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/24B3PAQW2ZSABNHTZ2EXOCJXZA","json":"https://pith.science/pith/24B3PAQW2ZSABNHTZ2EXOCJXZA.json","graph_json":"https://pith.science/api/pith-number/24B3PAQW2ZSABNHTZ2EXOCJXZA/graph.json","events_json":"https://pith.science/api/pith-number/24B3PAQW2ZSABNHTZ2EXOCJXZA/events.json","paper":"https://pith.science/paper/24B3PAQW"},"agent_actions":{"view_html":"https://pith.science/pith/24B3PAQW2ZSABNHTZ2EXOCJXZA","download_json":"https://pith.science/pith/24B3PAQW2ZSABNHTZ2EXOCJXZA.json","view_paper":"https://pith.science/paper/24B3PAQW","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2108.12380&json=true","fetch_graph":"https://pith.science/api/pith-number/24B3PAQW2ZSABNHTZ2EXOCJXZA/graph.json","fetch_events":"https://pith.science/api/pith-number/24B3PAQW2ZSABNHTZ2EXOCJXZA/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/24B3PAQW2ZSABNHTZ2EXOCJXZA/action/timestamp_anchor","attest_storage":"https://pith.science/pith/24B3PAQW2ZSABNHTZ2EXOCJXZA/action/storage_attestation","attest_author":"https://pith.science/pith/24B3PAQW2ZSABNHTZ2EXOCJXZA/action/author_attestation","sign_citation":"https://pith.science/pith/24B3PAQW2ZSABNHTZ2EXOCJXZA/action/citation_signature","submit_replication":"https://pith.science/pith/24B3PAQW2ZSABNHTZ2EXOCJXZA/action/replication_record"}},"created_at":"2026-07-05T03:57:11.372950+00:00","updated_at":"2026-07-05T03:57:11.372950+00:00"}