{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2013:KHE2F4YMYT4V5FUVFWNOWMOEKT","short_pith_number":"pith:KHE2F4YM","schema_version":"1.0","canonical_sha256":"51c9a2f30cc4f95e96952d9aeb31c454c42c18d531d6c39739f16e1a79267d87","source":{"kind":"arxiv","id":"1311.5900","version":1},"attestation_state":"computed","paper":{"title":"Numerical simulations of super-critical black hole accretion flows in general relativity","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"A. Sadowski, A. Tchekhovskoy, J. C. McKinney, R. Narayan","submitted_at":"2013-11-22T21:06:28Z","abstract_excerpt":"A new general relativistic radiation magnetohydrodynamical code KORAL, is described, which employs the M1 scheme to close the radiation moment equations. The code has been successfully verified against a number of tests. Axisymmetric simulations of super-critical magnetized accretion on a non-rotating black hole (a=0.0) and a spinning black hole (a=0.9) are presented. The accretion rates in the two models are \\dot M = 100-200 \\dot M_Edd. These first general relativistic simulations of super-critical black hole accretion are potentially relevant to tidal disruption events and hyper-accreting su"},"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":"1311.5900","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2013-11-22T21:06:28Z","cross_cats_sorted":[],"title_canon_sha256":"7dfeb1462ea73e6a3a5d30f2ae4898f2263798f5254fdee9cd55068709dc56ae","abstract_canon_sha256":"5b06f3aa148dc58498bd28406feaad475cd94fa99bdfa32f9562292255873dec"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:57:08.069537Z","signature_b64":"GEgTcm5FKgmnkbcgbaq2JosgDAzWA22rAckV3/+nYa3OMDp08We/kjKczTCQfCI0ekasmu1S3NE7Hhld8N2kBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"51c9a2f30cc4f95e96952d9aeb31c454c42c18d531d6c39739f16e1a79267d87","last_reissued_at":"2026-05-18T02:57:08.069016Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:57:08.069016Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Numerical simulations of super-critical black hole accretion flows in general relativity","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"A. Sadowski, A. Tchekhovskoy, J. C. McKinney, R. Narayan","submitted_at":"2013-11-22T21:06:28Z","abstract_excerpt":"A new general relativistic radiation magnetohydrodynamical code KORAL, is described, which employs the M1 scheme to close the radiation moment equations. The code has been successfully verified against a number of tests. Axisymmetric simulations of super-critical magnetized accretion on a non-rotating black hole (a=0.0) and a spinning black hole (a=0.9) are presented. The accretion rates in the two models are \\dot M = 100-200 \\dot M_Edd. These first general relativistic simulations of super-critical black hole accretion are potentially relevant to tidal disruption events and hyper-accreting su"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1311.5900","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":""},"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":"1311.5900","created_at":"2026-05-18T02:57:08.069097+00:00"},{"alias_kind":"arxiv_version","alias_value":"1311.5900v1","created_at":"2026-05-18T02:57:08.069097+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1311.5900","created_at":"2026-05-18T02:57:08.069097+00:00"},{"alias_kind":"pith_short_12","alias_value":"KHE2F4YMYT4V","created_at":"2026-05-18T12:27:49.015174+00:00"},{"alias_kind":"pith_short_16","alias_value":"KHE2F4YMYT4V5FUV","created_at":"2026-05-18T12:27:49.015174+00:00"},{"alias_kind":"pith_short_8","alias_value":"KHE2F4YM","created_at":"2026-05-18T12:27:49.015174+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":4,"internal_anchor_count":4,"sample":[{"citing_arxiv_id":"2605.22918","citing_title":"Strong X-ray Variability of I Zwicky 1: Obscuration from Clumpy Accretion-Disk Winds","ref_index":38,"is_internal_anchor":true},{"citing_arxiv_id":"2601.11203","citing_title":"Little Red Dots as Hidden Neutrino Sources","ref_index":25,"is_internal_anchor":true},{"citing_arxiv_id":"2605.13890","citing_title":"Analytic thin disks and rings in a class of nonasymptotically flat static spacetimes","ref_index":211,"is_internal_anchor":true},{"citing_arxiv_id":"2605.15166","citing_title":"Polarization Signatures from GRMHD Simulations of Black Hole Accretion","ref_index":20,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/KHE2F4YMYT4V5FUVFWNOWMOEKT","json":"https://pith.science/pith/KHE2F4YMYT4V5FUVFWNOWMOEKT.json","graph_json":"https://pith.science/api/pith-number/KHE2F4YMYT4V5FUVFWNOWMOEKT/graph.json","events_json":"https://pith.science/api/pith-number/KHE2F4YMYT4V5FUVFWNOWMOEKT/events.json","paper":"https://pith.science/paper/KHE2F4YM"},"agent_actions":{"view_html":"https://pith.science/pith/KHE2F4YMYT4V5FUVFWNOWMOEKT","download_json":"https://pith.science/pith/KHE2F4YMYT4V5FUVFWNOWMOEKT.json","view_paper":"https://pith.science/paper/KHE2F4YM","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1311.5900&json=true","fetch_graph":"https://pith.science/api/pith-number/KHE2F4YMYT4V5FUVFWNOWMOEKT/graph.json","fetch_events":"https://pith.science/api/pith-number/KHE2F4YMYT4V5FUVFWNOWMOEKT/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/KHE2F4YMYT4V5FUVFWNOWMOEKT/action/timestamp_anchor","attest_storage":"https://pith.science/pith/KHE2F4YMYT4V5FUVFWNOWMOEKT/action/storage_attestation","attest_author":"https://pith.science/pith/KHE2F4YMYT4V5FUVFWNOWMOEKT/action/author_attestation","sign_citation":"https://pith.science/pith/KHE2F4YMYT4V5FUVFWNOWMOEKT/action/citation_signature","submit_replication":"https://pith.science/pith/KHE2F4YMYT4V5FUVFWNOWMOEKT/action/replication_record"}},"created_at":"2026-05-18T02:57:08.069097+00:00","updated_at":"2026-05-18T02:57:08.069097+00:00"}