{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2009:KFXP7RXST6IG2KRF2LRN45V72Z","short_pith_number":"pith:KFXP7RXS","schema_version":"1.0","canonical_sha256":"516effc6f29f906d2a25d2e2de76bfd6686981bf991f7ba716a83a36322a4384","source":{"kind":"arxiv","id":"0906.2784","version":2},"attestation_state":"computed","paper":{"title":"Transport of Large Scale Poloidal Flux in Black Hole Accretion","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"John F. Hawley, Julian H. Krolik, Kris Beckwith","submitted_at":"2009-06-15T20:18:46Z","abstract_excerpt":"We report on a global, three-dimensional GRMHD simulation of an accretion torus embedded in a large scale vertical magnetic field orbiting a Schwarzschild black hole. This simulation investigates how a large scale vertical field evolves within a turbulent accretion disk and whether global magnetic field configurations suitable for launching jets and winds can develop. We find that a \"coronal mechanism\" of magnetic flux motion, which operates largely outside the disk body, dominates global flux evolution. In this mechanism, magnetic stresses driven by orbital shear create large-scale half-loops"},"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":"0906.2784","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2009-06-15T20:18:46Z","cross_cats_sorted":[],"title_canon_sha256":"74346bf876a0daf76a184794574cc18599bef902c5bd212f22bdacdfcdd52499","abstract_canon_sha256":"a295e6d2b127b28e92fce48cc39abbb2e2477fcea2f5fb82d5459cb67a3b5283"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T04:29:42.728165Z","signature_b64":"dxnH1CIvHNdLgZWWlygQdMkaKIUETMd7U1LKYMYfARDDiNxpc1+met/MXzDCCTmnyw13nOsGE7taAEazg/FaDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"516effc6f29f906d2a25d2e2de76bfd6686981bf991f7ba716a83a36322a4384","last_reissued_at":"2026-05-18T04:29:42.727771Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T04:29:42.727771Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Transport of Large Scale Poloidal Flux in Black Hole Accretion","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"John F. Hawley, Julian H. Krolik, Kris Beckwith","submitted_at":"2009-06-15T20:18:46Z","abstract_excerpt":"We report on a global, three-dimensional GRMHD simulation of an accretion torus embedded in a large scale vertical magnetic field orbiting a Schwarzschild black hole. This simulation investigates how a large scale vertical field evolves within a turbulent accretion disk and whether global magnetic field configurations suitable for launching jets and winds can develop. We find that a \"coronal mechanism\" of magnetic flux motion, which operates largely outside the disk body, dominates global flux evolution. In this mechanism, magnetic stresses driven by orbital shear create large-scale half-loops"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0906.2784","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":""},"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":"0906.2784","created_at":"2026-05-18T04:29:42.727827+00:00"},{"alias_kind":"arxiv_version","alias_value":"0906.2784v2","created_at":"2026-05-18T04:29:42.727827+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0906.2784","created_at":"2026-05-18T04:29:42.727827+00:00"},{"alias_kind":"pith_short_12","alias_value":"KFXP7RXST6IG","created_at":"2026-05-18T12:26:00.592388+00:00"},{"alias_kind":"pith_short_16","alias_value":"KFXP7RXST6IG2KRF","created_at":"2026-05-18T12:26:00.592388+00:00"},{"alias_kind":"pith_short_8","alias_value":"KFXP7RXS","created_at":"2026-05-18T12:26:00.592388+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":3,"sample":[{"citing_arxiv_id":"2605.19473","citing_title":"Radio-X-ray Time Lags in GX 339-4: Probing Magnetic Field Transport in Black Hole Accretion","ref_index":172,"is_internal_anchor":true},{"citing_arxiv_id":"2605.20317","citing_title":"Simulation-Based Prediction of Black Hole Fe K$\\alpha$ Line Profiles","ref_index":96,"is_internal_anchor":true},{"citing_arxiv_id":"2605.19473","citing_title":"Radio-X-ray Time Lags in GX 339-4: Probing Magnetic Field Transport in Black Hole Accretion","ref_index":172,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/KFXP7RXST6IG2KRF2LRN45V72Z","json":"https://pith.science/pith/KFXP7RXST6IG2KRF2LRN45V72Z.json","graph_json":"https://pith.science/api/pith-number/KFXP7RXST6IG2KRF2LRN45V72Z/graph.json","events_json":"https://pith.science/api/pith-number/KFXP7RXST6IG2KRF2LRN45V72Z/events.json","paper":"https://pith.science/paper/KFXP7RXS"},"agent_actions":{"view_html":"https://pith.science/pith/KFXP7RXST6IG2KRF2LRN45V72Z","download_json":"https://pith.science/pith/KFXP7RXST6IG2KRF2LRN45V72Z.json","view_paper":"https://pith.science/paper/KFXP7RXS","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0906.2784&json=true","fetch_graph":"https://pith.science/api/pith-number/KFXP7RXST6IG2KRF2LRN45V72Z/graph.json","fetch_events":"https://pith.science/api/pith-number/KFXP7RXST6IG2KRF2LRN45V72Z/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/KFXP7RXST6IG2KRF2LRN45V72Z/action/timestamp_anchor","attest_storage":"https://pith.science/pith/KFXP7RXST6IG2KRF2LRN45V72Z/action/storage_attestation","attest_author":"https://pith.science/pith/KFXP7RXST6IG2KRF2LRN45V72Z/action/author_attestation","sign_citation":"https://pith.science/pith/KFXP7RXST6IG2KRF2LRN45V72Z/action/citation_signature","submit_replication":"https://pith.science/pith/KFXP7RXST6IG2KRF2LRN45V72Z/action/replication_record"}},"created_at":"2026-05-18T04:29:42.727827+00:00","updated_at":"2026-05-18T04:29:42.727827+00:00"}