{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2016:HJ6P73INRRQFO4CPPJ4KS7MSEV","short_pith_number":"pith:HJ6P73IN","schema_version":"1.0","canonical_sha256":"3a7cffed0d8c6057704f7a78a97d9225739653fe2f87923866dc6be466c1142c","source":{"kind":"arxiv","id":"1601.05550","version":1},"attestation_state":"computed","paper":{"title":"Probing the magnetic field structure in Sgr A* on Black Hole Horizon Scales with Polarized Radiative Transfer Simulations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.HE","authors_text":"(2) Harvard-Smithsonian Center for Astrophysics, 3) ((1) Department of Physics & Joint Space-Science Institute, (3) Massachusetts Institute of Technology, Haystack Observatory), Jonathan C. McKinney (1), Michael D. Johnson (2), Roman Gold (1), Sheperd S. Doeleman (2, University of Maryland","submitted_at":"2016-01-21T08:47:13Z","abstract_excerpt":"Magnetic fields are believed to drive accretion and relativistic jets in black hole accretion systems, but the magnetic-field structure that controls these phenomena remains uncertain. We perform general relativistic (GR) polarized radiative transfer of time-dependent three-dimensional GR magnetohydrodynamical (MHD) simulations to model thermal synchrotron emission from the Galactic Center source Sagittarius A$^\\ast$ (Sgr A*). We compare our results to new polarimetry measurements by the Event Horizon Telescope (EHT) and show how polarization in the visibility (Fourier) domain distinguishes an"},"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":"1601.05550","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2016-01-21T08:47:13Z","cross_cats_sorted":["gr-qc"],"title_canon_sha256":"d9899eac1a4327d12b92e83c6e3957b1c4f91748571a0a705ffa4532865e10bb","abstract_canon_sha256":"0a5ed9a12750090ce5bdc383b795bb84188afbe828e49cc6f9538c79555ab4b7"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:48:20.266201Z","signature_b64":"bzNl1C3nDBlvodQt8KOHPFr4OGlsuq9ytxGmDXSE4OXeSIJo9zyOriuxN+okPpr9DgKs2APJr9bWvNgb54VBDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"3a7cffed0d8c6057704f7a78a97d9225739653fe2f87923866dc6be466c1142c","last_reissued_at":"2026-05-18T00:48:20.265522Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:48:20.265522Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Probing the magnetic field structure in Sgr A* on Black Hole Horizon Scales with Polarized Radiative Transfer Simulations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.HE","authors_text":"(2) Harvard-Smithsonian Center for Astrophysics, 3) ((1) Department of Physics & Joint Space-Science Institute, (3) Massachusetts Institute of Technology, Haystack Observatory), Jonathan C. McKinney (1), Michael D. Johnson (2), Roman Gold (1), Sheperd S. Doeleman (2, University of Maryland","submitted_at":"2016-01-21T08:47:13Z","abstract_excerpt":"Magnetic fields are believed to drive accretion and relativistic jets in black hole accretion systems, but the magnetic-field structure that controls these phenomena remains uncertain. We perform general relativistic (GR) polarized radiative transfer of time-dependent three-dimensional GR magnetohydrodynamical (MHD) simulations to model thermal synchrotron emission from the Galactic Center source Sagittarius A$^\\ast$ (Sgr A*). We compare our results to new polarimetry measurements by the Event Horizon Telescope (EHT) and show how polarization in the visibility (Fourier) domain distinguishes an"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1601.05550","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":"1601.05550","created_at":"2026-05-18T00:48:20.265648+00:00"},{"alias_kind":"arxiv_version","alias_value":"1601.05550v1","created_at":"2026-05-18T00:48:20.265648+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1601.05550","created_at":"2026-05-18T00:48:20.265648+00:00"},{"alias_kind":"pith_short_12","alias_value":"HJ6P73INRRQF","created_at":"2026-05-18T12:30:19.053100+00:00"},{"alias_kind":"pith_short_16","alias_value":"HJ6P73INRRQFO4CP","created_at":"2026-05-18T12:30:19.053100+00:00"},{"alias_kind":"pith_short_8","alias_value":"HJ6P73IN","created_at":"2026-05-18T12:30:19.053100+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":132,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/HJ6P73INRRQFO4CPPJ4KS7MSEV","json":"https://pith.science/pith/HJ6P73INRRQFO4CPPJ4KS7MSEV.json","graph_json":"https://pith.science/api/pith-number/HJ6P73INRRQFO4CPPJ4KS7MSEV/graph.json","events_json":"https://pith.science/api/pith-number/HJ6P73INRRQFO4CPPJ4KS7MSEV/events.json","paper":"https://pith.science/paper/HJ6P73IN"},"agent_actions":{"view_html":"https://pith.science/pith/HJ6P73INRRQFO4CPPJ4KS7MSEV","download_json":"https://pith.science/pith/HJ6P73INRRQFO4CPPJ4KS7MSEV.json","view_paper":"https://pith.science/paper/HJ6P73IN","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1601.05550&json=true","fetch_graph":"https://pith.science/api/pith-number/HJ6P73INRRQFO4CPPJ4KS7MSEV/graph.json","fetch_events":"https://pith.science/api/pith-number/HJ6P73INRRQFO4CPPJ4KS7MSEV/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/HJ6P73INRRQFO4CPPJ4KS7MSEV/action/timestamp_anchor","attest_storage":"https://pith.science/pith/HJ6P73INRRQFO4CPPJ4KS7MSEV/action/storage_attestation","attest_author":"https://pith.science/pith/HJ6P73INRRQFO4CPPJ4KS7MSEV/action/author_attestation","sign_citation":"https://pith.science/pith/HJ6P73INRRQFO4CPPJ4KS7MSEV/action/citation_signature","submit_replication":"https://pith.science/pith/HJ6P73INRRQFO4CPPJ4KS7MSEV/action/replication_record"}},"created_at":"2026-05-18T00:48:20.265648+00:00","updated_at":"2026-05-18T00:48:20.265648+00:00"}