{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2010:ZPINZGEMZ5SDIJYCONL7AUYTKG","short_pith_number":"pith:ZPINZGEM","schema_version":"1.0","canonical_sha256":"cbd0dc988ccf643427027357f0531351bfb8140085fe558d9aca18373adcfe13","source":{"kind":"arxiv","id":"1006.5015","version":1},"attestation_state":"computed","paper":{"title":"Parsec-scale Faraday Rotation Measures from General Relativistic MHD Simulations of Active Galactic Nuclei Jets","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"(2) KIPAC), Avery E. Broderick(1), Jonathan C. McKinney(2) ((1) CITA","submitted_at":"2010-06-25T16:05:02Z","abstract_excerpt":"For the first time it has become possible to compare global 3D general relativistic magnetohydrodynamic (GRMHD) jet formation simulations directly to very-long baseline interferometric multi-frequency polarization observations of the pc-scale structure of active galactic nucleus (AGN) jets. Unlike the jet emission, which requires post hoc modeling of the non-thermal electrons, the Faraday rotation measures (RMs) depend primarily upon simulated quantities and thus provide a robust way in which to confront simulations with observations. We compute RM distributions of 3D global GRMHD jet formatio"},"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":"1006.5015","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2010-06-25T16:05:02Z","cross_cats_sorted":[],"title_canon_sha256":"ad198160209b9817f8f473150066fc953ac2221f68753d5c06c4ea9f0bd20b52","abstract_canon_sha256":"9144425dfd0efe5c04c37f0bd271bce05cfffa5e6f09447a076cc437d1956e44"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T02:06:42.333548Z","signature_b64":"y/W8IFAbuuYEm4cPf6hlgIZdbBXeHmpbDRGYSl6va9puj7d/FoUe+mSllwDe+cYsNaUYQ+5ZdYpC6eju43MWBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"cbd0dc988ccf643427027357f0531351bfb8140085fe558d9aca18373adcfe13","last_reissued_at":"2026-05-18T02:06:42.333023Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T02:06:42.333023Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Parsec-scale Faraday Rotation Measures from General Relativistic MHD Simulations of Active Galactic Nuclei Jets","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"(2) KIPAC), Avery E. Broderick(1), Jonathan C. McKinney(2) ((1) CITA","submitted_at":"2010-06-25T16:05:02Z","abstract_excerpt":"For the first time it has become possible to compare global 3D general relativistic magnetohydrodynamic (GRMHD) jet formation simulations directly to very-long baseline interferometric multi-frequency polarization observations of the pc-scale structure of active galactic nucleus (AGN) jets. Unlike the jet emission, which requires post hoc modeling of the non-thermal electrons, the Faraday rotation measures (RMs) depend primarily upon simulated quantities and thus provide a robust way in which to confront simulations with observations. We compute RM distributions of 3D global GRMHD jet formatio"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1006.5015","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":"1006.5015","created_at":"2026-05-18T02:06:42.333108+00:00"},{"alias_kind":"arxiv_version","alias_value":"1006.5015v1","created_at":"2026-05-18T02:06:42.333108+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1006.5015","created_at":"2026-05-18T02:06:42.333108+00:00"},{"alias_kind":"pith_short_12","alias_value":"ZPINZGEMZ5SD","created_at":"2026-05-18T12:26:18.847500+00:00"},{"alias_kind":"pith_short_16","alias_value":"ZPINZGEMZ5SDIJYC","created_at":"2026-05-18T12:26:18.847500+00:00"},{"alias_kind":"pith_short_8","alias_value":"ZPINZGEM","created_at":"2026-05-18T12:26:18.847500+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.15166","citing_title":"Polarization Signatures from GRMHD Simulations of Black Hole Accretion","ref_index":130,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/ZPINZGEMZ5SDIJYCONL7AUYTKG","json":"https://pith.science/pith/ZPINZGEMZ5SDIJYCONL7AUYTKG.json","graph_json":"https://pith.science/api/pith-number/ZPINZGEMZ5SDIJYCONL7AUYTKG/graph.json","events_json":"https://pith.science/api/pith-number/ZPINZGEMZ5SDIJYCONL7AUYTKG/events.json","paper":"https://pith.science/paper/ZPINZGEM"},"agent_actions":{"view_html":"https://pith.science/pith/ZPINZGEMZ5SDIJYCONL7AUYTKG","download_json":"https://pith.science/pith/ZPINZGEMZ5SDIJYCONL7AUYTKG.json","view_paper":"https://pith.science/paper/ZPINZGEM","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1006.5015&json=true","fetch_graph":"https://pith.science/api/pith-number/ZPINZGEMZ5SDIJYCONL7AUYTKG/graph.json","fetch_events":"https://pith.science/api/pith-number/ZPINZGEMZ5SDIJYCONL7AUYTKG/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/ZPINZGEMZ5SDIJYCONL7AUYTKG/action/timestamp_anchor","attest_storage":"https://pith.science/pith/ZPINZGEMZ5SDIJYCONL7AUYTKG/action/storage_attestation","attest_author":"https://pith.science/pith/ZPINZGEMZ5SDIJYCONL7AUYTKG/action/author_attestation","sign_citation":"https://pith.science/pith/ZPINZGEMZ5SDIJYCONL7AUYTKG/action/citation_signature","submit_replication":"https://pith.science/pith/ZPINZGEMZ5SDIJYCONL7AUYTKG/action/replication_record"}},"created_at":"2026-05-18T02:06:42.333108+00:00","updated_at":"2026-05-18T02:06:42.333108+00:00"}