{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2007:EFIMUV65GPZQ523TN6QOSF7EPS","short_pith_number":"pith:EFIMUV65","schema_version":"1.0","canonical_sha256":"2150ca57dd33f30eeb736fa0e917e47c9e34028e633f044319d4340235db1313","source":{"kind":"arxiv","id":"0705.3622","version":2},"attestation_state":"computed","paper":{"title":"MHD simulations of the magnetorotational instability in a shearing box with zero net flux. II. The effect of transport coefficients","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"G. Lesur, J. Papaloizou, S. Fromang, T. Heinemann","submitted_at":"2007-05-24T17:02:26Z","abstract_excerpt":"We study the influence of the choice of transport coefficients (viscosity and resistivity) on MHD turbulence driven by the magnetorotational instability (MRI) in accretion disks. We follow the methodology described in paper I: we adopt an unstratified shearing box model and focus on the case where the net vertical magnetic flux threading the box vanishes. For the most part we use the finite difference code ZEUS, including explicit transport coefficients in the calculations. However, we also compare our results with those obtained using other algorithms (NIRVANA, the PENCIL code and a spectral "},"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":"0705.3622","kind":"arxiv","version":2},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2007-05-24T17:02:26Z","cross_cats_sorted":[],"title_canon_sha256":"09fd4179c9185fa7d34024ef1ad1f35b13f6ac48224701bdde16c2f193230862","abstract_canon_sha256":"4c8a506010d3b706c5d41be241a2a9b29e22188fa0990a84f0d80ab727970b72"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-04T17:03:57.739564Z","signature_b64":"nQe613TT87lQRITdknU0rVkgYHPrIoZp2+s1T8aT7Jxs/WkrPPVYPh1W0oTyywbr2Hrsp+3W8KuARpEbu65KDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"2150ca57dd33f30eeb736fa0e917e47c9e34028e633f044319d4340235db1313","last_reissued_at":"2026-07-04T17:03:57.739171Z","signature_status":"signed_v1","first_computed_at":"2026-07-04T17:03:57.739171Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"MHD simulations of the magnetorotational instability in a shearing box with zero net flux. II. The effect of transport coefficients","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"G. Lesur, J. Papaloizou, S. Fromang, T. Heinemann","submitted_at":"2007-05-24T17:02:26Z","abstract_excerpt":"We study the influence of the choice of transport coefficients (viscosity and resistivity) on MHD turbulence driven by the magnetorotational instability (MRI) in accretion disks. We follow the methodology described in paper I: we adopt an unstratified shearing box model and focus on the case where the net vertical magnetic flux threading the box vanishes. For the most part we use the finite difference code ZEUS, including explicit transport coefficients in the calculations. However, we also compare our results with those obtained using other algorithms (NIRVANA, the PENCIL code and a spectral "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0705.3622","kind":"arxiv","version":2},"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/0705.3622/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":"0705.3622","created_at":"2026-07-04T17:03:57.739226+00:00"},{"alias_kind":"arxiv_version","alias_value":"0705.3622v2","created_at":"2026-07-04T17:03:57.739226+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0705.3622","created_at":"2026-07-04T17:03:57.739226+00:00"},{"alias_kind":"pith_short_12","alias_value":"EFIMUV65GPZQ","created_at":"2026-07-04T17:03:57.739226+00:00"},{"alias_kind":"pith_short_16","alias_value":"EFIMUV65GPZQ523T","created_at":"2026-07-04T17:03:57.739226+00:00"},{"alias_kind":"pith_short_8","alias_value":"EFIMUV65","created_at":"2026-07-04T17:03:57.739226+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":2,"sample":[{"citing_arxiv_id":"2605.02996","citing_title":"Wave interference as the origin of the cyclic magnetorotational dynamo in accretion disks: insights from weakly nonlinear theory and local shearing box simulations","ref_index":23,"is_internal_anchor":true},{"citing_arxiv_id":"2605.02996","citing_title":"Wave interference as the origin of the cyclic magnetorotational dynamo in accretion disks: insights from weakly nonlinear theory and local shearing box simulations","ref_index":22,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/EFIMUV65GPZQ523TN6QOSF7EPS","json":"https://pith.science/pith/EFIMUV65GPZQ523TN6QOSF7EPS.json","graph_json":"https://pith.science/api/pith-number/EFIMUV65GPZQ523TN6QOSF7EPS/graph.json","events_json":"https://pith.science/api/pith-number/EFIMUV65GPZQ523TN6QOSF7EPS/events.json","paper":"https://pith.science/paper/EFIMUV65"},"agent_actions":{"view_html":"https://pith.science/pith/EFIMUV65GPZQ523TN6QOSF7EPS","download_json":"https://pith.science/pith/EFIMUV65GPZQ523TN6QOSF7EPS.json","view_paper":"https://pith.science/paper/EFIMUV65","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0705.3622&json=true","fetch_graph":"https://pith.science/api/pith-number/EFIMUV65GPZQ523TN6QOSF7EPS/graph.json","fetch_events":"https://pith.science/api/pith-number/EFIMUV65GPZQ523TN6QOSF7EPS/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/EFIMUV65GPZQ523TN6QOSF7EPS/action/timestamp_anchor","attest_storage":"https://pith.science/pith/EFIMUV65GPZQ523TN6QOSF7EPS/action/storage_attestation","attest_author":"https://pith.science/pith/EFIMUV65GPZQ523TN6QOSF7EPS/action/author_attestation","sign_citation":"https://pith.science/pith/EFIMUV65GPZQ523TN6QOSF7EPS/action/citation_signature","submit_replication":"https://pith.science/pith/EFIMUV65GPZQ523TN6QOSF7EPS/action/replication_record"}},"created_at":"2026-07-04T17:03:57.739226+00:00","updated_at":"2026-07-04T17:03:57.739226+00:00"}