{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2015:5UFR3B5POYGOBGZPWQWTMNWHYV","short_pith_number":"pith:5UFR3B5P","schema_version":"1.0","canonical_sha256":"ed0b1d87af760ce09b2fb42d3636c7c56cbde240b1d96cd139ae697dfb100e86","source":{"kind":"arxiv","id":"1510.07243","version":3},"attestation_state":"computed","paper":{"title":"General relativistic magnetohydrodynamical simulations of the jet in M87","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Heino Falcke, Hotaka Shiokawa, Monika Moscibrodzka","submitted_at":"2015-10-25T13:25:02Z","abstract_excerpt":"(abridged) The connection between black hole, accretion disk, and radio jet can be best constrained by fitting models to observations of nearby low luminosity galactic nuclei, in particular the well studied sources Sgr~A* and M87. There has been considerable progress in modeling the central engine of active galactic nuclei by an accreting supermassive black hole coupled to a relativistic plasma jet. However, can a single model be applied to a range of black hole masses and accretion rates? Here we want to compare the latest three-dimensional numerical model, originally developed for Sgr A* in "},"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":"1510.07243","kind":"arxiv","version":3},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2015-10-25T13:25:02Z","cross_cats_sorted":[],"title_canon_sha256":"17d6d370268d5253a2ef84da02fea3a657b3c0679b37080fea1df9cec661c48d","abstract_canon_sha256":"ae7128eaa419cdb3a31158de8b43410cf1aa4852dc2b00ab68924db06bd59c00"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:16:02.666514Z","signature_b64":"a+bTeb4FZ0mZ+AaaoLCiBdxAvkLPxmU6yLQNaP7ZMYSCJwgk7ijNEDX+tjbgZwPxFRU3Rw1sdYpv/WkloLbJBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"ed0b1d87af760ce09b2fb42d3636c7c56cbde240b1d96cd139ae697dfb100e86","last_reissued_at":"2026-05-18T01:16:02.665808Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:16:02.665808Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"General relativistic magnetohydrodynamical simulations of the jet in M87","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Heino Falcke, Hotaka Shiokawa, Monika Moscibrodzka","submitted_at":"2015-10-25T13:25:02Z","abstract_excerpt":"(abridged) The connection between black hole, accretion disk, and radio jet can be best constrained by fitting models to observations of nearby low luminosity galactic nuclei, in particular the well studied sources Sgr~A* and M87. There has been considerable progress in modeling the central engine of active galactic nuclei by an accreting supermassive black hole coupled to a relativistic plasma jet. However, can a single model be applied to a range of black hole masses and accretion rates? Here we want to compare the latest three-dimensional numerical model, originally developed for Sgr A* in "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1510.07243","kind":"arxiv","version":3},"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":"1510.07243","created_at":"2026-05-18T01:16:02.665916+00:00"},{"alias_kind":"arxiv_version","alias_value":"1510.07243v3","created_at":"2026-05-18T01:16:02.665916+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1510.07243","created_at":"2026-05-18T01:16:02.665916+00:00"},{"alias_kind":"pith_short_12","alias_value":"5UFR3B5POYGO","created_at":"2026-05-18T12:29:07.941421+00:00"},{"alias_kind":"pith_short_16","alias_value":"5UFR3B5POYGOBGZP","created_at":"2026-05-18T12:29:07.941421+00:00"},{"alias_kind":"pith_short_8","alias_value":"5UFR3B5P","created_at":"2026-05-18T12:29:07.941421+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2605.15166","citing_title":"Polarization Signatures from GRMHD Simulations of Black Hole Accretion","ref_index":164,"is_internal_anchor":true},{"citing_arxiv_id":"2604.15430","citing_title":"GRMHD accretion beyond the black hole paradigm: Light from within the shadow","ref_index":57,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/5UFR3B5POYGOBGZPWQWTMNWHYV","json":"https://pith.science/pith/5UFR3B5POYGOBGZPWQWTMNWHYV.json","graph_json":"https://pith.science/api/pith-number/5UFR3B5POYGOBGZPWQWTMNWHYV/graph.json","events_json":"https://pith.science/api/pith-number/5UFR3B5POYGOBGZPWQWTMNWHYV/events.json","paper":"https://pith.science/paper/5UFR3B5P"},"agent_actions":{"view_html":"https://pith.science/pith/5UFR3B5POYGOBGZPWQWTMNWHYV","download_json":"https://pith.science/pith/5UFR3B5POYGOBGZPWQWTMNWHYV.json","view_paper":"https://pith.science/paper/5UFR3B5P","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1510.07243&json=true","fetch_graph":"https://pith.science/api/pith-number/5UFR3B5POYGOBGZPWQWTMNWHYV/graph.json","fetch_events":"https://pith.science/api/pith-number/5UFR3B5POYGOBGZPWQWTMNWHYV/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/5UFR3B5POYGOBGZPWQWTMNWHYV/action/timestamp_anchor","attest_storage":"https://pith.science/pith/5UFR3B5POYGOBGZPWQWTMNWHYV/action/storage_attestation","attest_author":"https://pith.science/pith/5UFR3B5POYGOBGZPWQWTMNWHYV/action/author_attestation","sign_citation":"https://pith.science/pith/5UFR3B5POYGOBGZPWQWTMNWHYV/action/citation_signature","submit_replication":"https://pith.science/pith/5UFR3B5POYGOBGZPWQWTMNWHYV/action/replication_record"}},"created_at":"2026-05-18T01:16:02.665916+00:00","updated_at":"2026-05-18T01:16:02.665916+00:00"}