{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2006:AM2URNUJQY44M6ZOTFVCDBJQDQ","short_pith_number":"pith:AM2URNUJ","schema_version":"1.0","canonical_sha256":"033548b6898639c67b2e996a2185301c10363cd5638f1fbd4fdcbbd23af1f356","source":{"kind":"arxiv","id":"astro-ph/0607576","version":3},"attestation_state":"computed","paper":{"title":"Disk-Jet Coupling in Black Hole Accretion Systems II: Force-Free Electrodynamical Models","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"2) ((1) Institute for Theory, (2) Harvard University), Computation, Jonathan C. McKinney (1), Ramesh Narayan (1","submitted_at":"2006-07-26T10:57:09Z","abstract_excerpt":"In paper I, we showed that time-dependent general relativistic magnetohydrodynamic (GRMHD) numerical models of accretion disks, although being highly turbulent, have surprisingly simple electromagnetic properties. In particular, the toroidal current density in the disk takes the form $dI_\\phi/dr \\propto r^{-5/4}$. Guided by this simplicity, we use a time-dependent general relativistic force-free electrodynamics (GRFFE) code to study an idealized problem in which the accretion disk is replaced by an infinitely thin rotating equatorial current sheet. We consider both an $r^{-5/4}$ current profil"},"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/0607576","kind":"arxiv","version":3},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2006-07-26T10:57:09Z","cross_cats_sorted":[],"title_canon_sha256":"90b6e22082182591bd775ed0f50dc8dc13035782324ad542a347979fc409ca16","abstract_canon_sha256":"f0ade8aacfface43bb4f2e7f56bf2931b89f5b66d6ce00f31fad2990cb5010f5"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T15:16:50.548822Z","signature_b64":"xcItdsqN7MsNNGUiHlZYhm2JqzALbCvsRv2t91RAawqiypLawJ6Iy3a5hIR/5nn9ApBpbCm2rJV9wnn+tIHmAw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"033548b6898639c67b2e996a2185301c10363cd5638f1fbd4fdcbbd23af1f356","last_reissued_at":"2026-07-04T15:16:50.548428Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T15:16:50.548428Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Disk-Jet Coupling in Black Hole Accretion Systems II: Force-Free Electrodynamical Models","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"2) ((1) Institute for Theory, (2) Harvard University), Computation, Jonathan C. McKinney (1), Ramesh Narayan (1","submitted_at":"2006-07-26T10:57:09Z","abstract_excerpt":"In paper I, we showed that time-dependent general relativistic magnetohydrodynamic (GRMHD) numerical models of accretion disks, although being highly turbulent, have surprisingly simple electromagnetic properties. In particular, the toroidal current density in the disk takes the form $dI_\\phi/dr \\propto r^{-5/4}$. Guided by this simplicity, we use a time-dependent general relativistic force-free electrodynamics (GRFFE) code to study an idealized problem in which the accretion disk is replaced by an infinitely thin rotating equatorial current sheet. We consider both an $r^{-5/4}$ current profil"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0607576","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/astro-ph/0607576/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/0607576","created_at":"2026-07-04T15:16:50.548496+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0607576v3","created_at":"2026-07-04T15:16:50.548496+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0607576","created_at":"2026-07-04T15:16:50.548496+00:00"},{"alias_kind":"pith_short_12","alias_value":"AM2URNUJQY44","created_at":"2026-07-04T15:16:50.548496+00:00"},{"alias_kind":"pith_short_16","alias_value":"AM2URNUJQY44M6ZO","created_at":"2026-07-04T15:16:50.548496+00:00"},{"alias_kind":"pith_short_8","alias_value":"AM2URNUJ","created_at":"2026-07-04T15:16:50.548496+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2604.27797","citing_title":"Magnetic reconnection in five-dimensional Kerr black hole","ref_index":16,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/AM2URNUJQY44M6ZOTFVCDBJQDQ","json":"https://pith.science/pith/AM2URNUJQY44M6ZOTFVCDBJQDQ.json","graph_json":"https://pith.science/api/pith-number/AM2URNUJQY44M6ZOTFVCDBJQDQ/graph.json","events_json":"https://pith.science/api/pith-number/AM2URNUJQY44M6ZOTFVCDBJQDQ/events.json","paper":"https://pith.science/paper/AM2URNUJ"},"agent_actions":{"view_html":"https://pith.science/pith/AM2URNUJQY44M6ZOTFVCDBJQDQ","download_json":"https://pith.science/pith/AM2URNUJQY44M6ZOTFVCDBJQDQ.json","view_paper":"https://pith.science/paper/AM2URNUJ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0607576&json=true","fetch_graph":"https://pith.science/api/pith-number/AM2URNUJQY44M6ZOTFVCDBJQDQ/graph.json","fetch_events":"https://pith.science/api/pith-number/AM2URNUJQY44M6ZOTFVCDBJQDQ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/AM2URNUJQY44M6ZOTFVCDBJQDQ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/AM2URNUJQY44M6ZOTFVCDBJQDQ/action/storage_attestation","attest_author":"https://pith.science/pith/AM2URNUJQY44M6ZOTFVCDBJQDQ/action/author_attestation","sign_citation":"https://pith.science/pith/AM2URNUJQY44M6ZOTFVCDBJQDQ/action/citation_signature","submit_replication":"https://pith.science/pith/AM2URNUJQY44M6ZOTFVCDBJQDQ/action/replication_record"}},"created_at":"2026-07-04T15:16:50.548496+00:00","updated_at":"2026-07-04T15:16:50.548496+00:00"}