{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2017:H7CMB2LV4ACRJLNHPA7OXP5MOI","short_pith_number":"pith:H7CMB2LV","schema_version":"1.0","canonical_sha256":"3fc4c0e975e00514ada7783eebbfac723c28f891a71b6b9be3b4f33e4b906562","source":{"kind":"arxiv","id":"1707.00983","version":1},"attestation_state":"computed","paper":{"title":"Magnetorotational Instability in Core-Collapse Supernovae","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.HE","authors_text":"E. M\\\"uller, J\\'er\\^ome Guilet, Martin Obergaulinger, Miguel-\\'Angel Aloy, Pablo Cerd\\'a-Dur\\'an, Tomasz Rembiasz","submitted_at":"2017-07-01T14:49:27Z","abstract_excerpt":"We discuss the relevance of the magnetorotational instability (MRI) in core-collapse supernovae (CCSNe). Our recent numerical studies show that in CCSNe, the MRI is terminated by parasitic instabilities of the Kelvin-Helmholtz type. To determine whether the MRI can amplify initially weak magnetic fields to dynamically relevant strengths in CCSNe, we performed three-dimensional simulations of a region close to the surface of a differentially rotating proto-neutron star in non-ideal magnetohydrodynamics with two different numerical codes. We find that under the conditions prevailing in proto-neu"},"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":"1707.00983","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2017-07-01T14:49:27Z","cross_cats_sorted":["astro-ph.SR"],"title_canon_sha256":"4cc8eec8b975e5ac6d9d04c1e6a17607d220c82bf8ecc23245830cc72d243535","abstract_canon_sha256":"142a1a0db5ad676eb1d6d622faa0d712e9704952daa55af038fde7083e504954"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T00:40:56.469567Z","signature_b64":"7kGyVhztZMsj2k2SlrLx1SeQ28Z5+FUcQUt+WYJKialhOhBNzDaF69mfo+nthu6tUmNzzy9cdVJB7OcOt9cBDA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"3fc4c0e975e00514ada7783eebbfac723c28f891a71b6b9be3b4f33e4b906562","last_reissued_at":"2026-05-18T00:40:56.468957Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T00:40:56.468957Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Magnetorotational Instability in Core-Collapse Supernovae","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"astro-ph.HE","authors_text":"E. M\\\"uller, J\\'er\\^ome Guilet, Martin Obergaulinger, Miguel-\\'Angel Aloy, Pablo Cerd\\'a-Dur\\'an, Tomasz Rembiasz","submitted_at":"2017-07-01T14:49:27Z","abstract_excerpt":"We discuss the relevance of the magnetorotational instability (MRI) in core-collapse supernovae (CCSNe). Our recent numerical studies show that in CCSNe, the MRI is terminated by parasitic instabilities of the Kelvin-Helmholtz type. To determine whether the MRI can amplify initially weak magnetic fields to dynamically relevant strengths in CCSNe, we performed three-dimensional simulations of a region close to the surface of a differentially rotating proto-neutron star in non-ideal magnetohydrodynamics with two different numerical codes. We find that under the conditions prevailing in proto-neu"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1707.00983","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":"1707.00983","created_at":"2026-05-18T00:40:56.469047+00:00"},{"alias_kind":"arxiv_version","alias_value":"1707.00983v1","created_at":"2026-05-18T00:40:56.469047+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1707.00983","created_at":"2026-05-18T00:40:56.469047+00:00"},{"alias_kind":"pith_short_12","alias_value":"H7CMB2LV4ACR","created_at":"2026-05-18T12:31:18.294218+00:00"},{"alias_kind":"pith_short_16","alias_value":"H7CMB2LV4ACRJLNH","created_at":"2026-05-18T12:31:18.294218+00:00"},{"alias_kind":"pith_short_8","alias_value":"H7CMB2LV","created_at":"2026-05-18T12:31:18.294218+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":0,"internal_anchor_count":0,"sample":[]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/H7CMB2LV4ACRJLNHPA7OXP5MOI","json":"https://pith.science/pith/H7CMB2LV4ACRJLNHPA7OXP5MOI.json","graph_json":"https://pith.science/api/pith-number/H7CMB2LV4ACRJLNHPA7OXP5MOI/graph.json","events_json":"https://pith.science/api/pith-number/H7CMB2LV4ACRJLNHPA7OXP5MOI/events.json","paper":"https://pith.science/paper/H7CMB2LV"},"agent_actions":{"view_html":"https://pith.science/pith/H7CMB2LV4ACRJLNHPA7OXP5MOI","download_json":"https://pith.science/pith/H7CMB2LV4ACRJLNHPA7OXP5MOI.json","view_paper":"https://pith.science/paper/H7CMB2LV","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1707.00983&json=true","fetch_graph":"https://pith.science/api/pith-number/H7CMB2LV4ACRJLNHPA7OXP5MOI/graph.json","fetch_events":"https://pith.science/api/pith-number/H7CMB2LV4ACRJLNHPA7OXP5MOI/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/H7CMB2LV4ACRJLNHPA7OXP5MOI/action/timestamp_anchor","attest_storage":"https://pith.science/pith/H7CMB2LV4ACRJLNHPA7OXP5MOI/action/storage_attestation","attest_author":"https://pith.science/pith/H7CMB2LV4ACRJLNHPA7OXP5MOI/action/author_attestation","sign_citation":"https://pith.science/pith/H7CMB2LV4ACRJLNHPA7OXP5MOI/action/citation_signature","submit_replication":"https://pith.science/pith/H7CMB2LV4ACRJLNHPA7OXP5MOI/action/replication_record"}},"created_at":"2026-05-18T00:40:56.469047+00:00","updated_at":"2026-05-18T00:40:56.469047+00:00"}