{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2006:2H6VUWYZTUURYEG776ESJAATMZ","short_pith_number":"pith:2H6VUWYZ","schema_version":"1.0","canonical_sha256":"d1fd5a5b199d291c10dfff89248013666a4cf6a16f0167a4e04d6c370c68edcc","source":{"kind":"arxiv","id":"astro-ph/0603045","version":1},"attestation_state":"computed","paper":{"title":"General Relativistic Magnetohydrodynamic Simulations of Jet Formation and Large-Scale Propagation from Black Hole Accretion Systems","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Computation, Harvard-Smithsonian Center for Astrophysics), Jonathan C. McKinney (Institute for Theory","submitted_at":"2006-03-02T20:40:43Z","abstract_excerpt":"The formation and large-scale propagation of Poynting-dominated jets produced by accreting, rapidly rotating black hole systems are studied by numerically integrating the general relativistic magnetohydrodynamic equations of motion to follow the self-consistent interaction between accretion disks and black holes. This study extends previous similar work by studying jets till $t\\approx 10^4GM/c^3$ out to $r\\approx 10^4GM/c^2$, by which the jet is super- fast magnetosonic and moves at a lab-frame bulk Lorentz factor of $\\Gamma\\sim 10$ with a maximum terminal Lorentz factor of $\\Gamma_\\infty\\less"},"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/0603045","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2006-03-02T20:40:43Z","cross_cats_sorted":[],"title_canon_sha256":"7798c190c344562199e81a96e34e2cd5e667a0c7072139f998e8d2f3efae7672","abstract_canon_sha256":"7bc993b4d16263c36e1bd288c28ed522e8b993dc87755263dd7a4397d00e58d7"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T17:25:16.209523Z","signature_b64":"FFOPRJFUFpUL6+34Sr772zVfhRrivnnmhWcHCNNGqx4BV5A1ozldtbKYQyzNI9Qo0DkhGVgNvTE59KQ+rJ0uCw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"d1fd5a5b199d291c10dfff89248013666a4cf6a16f0167a4e04d6c370c68edcc","last_reissued_at":"2026-07-04T17:25:16.209059Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T17:25:16.209059Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"General Relativistic Magnetohydrodynamic Simulations of Jet Formation and Large-Scale Propagation from Black Hole Accretion Systems","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"Computation, Harvard-Smithsonian Center for Astrophysics), Jonathan C. McKinney (Institute for Theory","submitted_at":"2006-03-02T20:40:43Z","abstract_excerpt":"The formation and large-scale propagation of Poynting-dominated jets produced by accreting, rapidly rotating black hole systems are studied by numerically integrating the general relativistic magnetohydrodynamic equations of motion to follow the self-consistent interaction between accretion disks and black holes. This study extends previous similar work by studying jets till $t\\approx 10^4GM/c^3$ out to $r\\approx 10^4GM/c^2$, by which the jet is super- fast magnetosonic and moves at a lab-frame bulk Lorentz factor of $\\Gamma\\sim 10$ with a maximum terminal Lorentz factor of $\\Gamma_\\infty\\less"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0603045","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/0603045/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/0603045","created_at":"2026-07-04T17:25:16.209125+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0603045v1","created_at":"2026-07-04T17:25:16.209125+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0603045","created_at":"2026-07-04T17:25:16.209125+00:00"},{"alias_kind":"pith_short_12","alias_value":"2H6VUWYZTUUR","created_at":"2026-07-04T17:25:16.209125+00:00"},{"alias_kind":"pith_short_16","alias_value":"2H6VUWYZTUURYEG7","created_at":"2026-07-04T17:25:16.209125+00:00"},{"alias_kind":"pith_short_8","alias_value":"2H6VUWYZ","created_at":"2026-07-04T17:25:16.209125+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2606.19320","citing_title":"GRMHD and GRRT Simulations of Black Hole Accretion: Flares, Precession, and Complex Spacetimes","ref_index":62,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/2H6VUWYZTUURYEG776ESJAATMZ","json":"https://pith.science/pith/2H6VUWYZTUURYEG776ESJAATMZ.json","graph_json":"https://pith.science/api/pith-number/2H6VUWYZTUURYEG776ESJAATMZ/graph.json","events_json":"https://pith.science/api/pith-number/2H6VUWYZTUURYEG776ESJAATMZ/events.json","paper":"https://pith.science/paper/2H6VUWYZ"},"agent_actions":{"view_html":"https://pith.science/pith/2H6VUWYZTUURYEG776ESJAATMZ","download_json":"https://pith.science/pith/2H6VUWYZTUURYEG776ESJAATMZ.json","view_paper":"https://pith.science/paper/2H6VUWYZ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0603045&json=true","fetch_graph":"https://pith.science/api/pith-number/2H6VUWYZTUURYEG776ESJAATMZ/graph.json","fetch_events":"https://pith.science/api/pith-number/2H6VUWYZTUURYEG776ESJAATMZ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/2H6VUWYZTUURYEG776ESJAATMZ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/2H6VUWYZTUURYEG776ESJAATMZ/action/storage_attestation","attest_author":"https://pith.science/pith/2H6VUWYZTUURYEG776ESJAATMZ/action/author_attestation","sign_citation":"https://pith.science/pith/2H6VUWYZTUURYEG776ESJAATMZ/action/citation_signature","submit_replication":"https://pith.science/pith/2H6VUWYZTUURYEG776ESJAATMZ/action/replication_record"}},"created_at":"2026-07-04T17:25:16.209125+00:00","updated_at":"2026-07-04T17:25:16.209125+00:00"}