{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:OQ23S2WP7WIYTBNZDI5KSQ6VPV","short_pith_number":"pith:OQ23S2WP","schema_version":"1.0","canonical_sha256":"7435b96acffd918985b91a3aa943d57d4b28fd9825762bad7be2aa36e2427131","source":{"kind":"arxiv","id":"2109.08732","version":1},"attestation_state":"computed","paper":{"title":"Long-term evolution of neutron-star merger remnants in general relativistic resistive-magnetohydrodynamics with a mean-field dynamo term","license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Masaru Shibata, Sho Fujibayashi, Yuichiro Sekiguchi","submitted_at":"2021-09-17T19:26:25Z","abstract_excerpt":"Long-term neutrino-radiation resistive-magnetohydrodynamics simulations in full general relativity are performed for a system composed of a massive neutron star and a torus formed as a remnant of binary neutron star mergers. The simulation is performed in axial symmetry incorporating a mean-field dynamo term for a hypothetical amplification of the magnetic-field strength. We first calibrate the mean-field dynamo parameters by comparing the results for the evolution of black hole-disk systems with viscous hydrodynamics results. We then perform simulations for the system of a remnant massive 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":"2109.08732","kind":"arxiv","version":1},"metadata":{"license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","primary_cat":"astro-ph.HE","submitted_at":"2021-09-17T19:26:25Z","cross_cats_sorted":[],"title_canon_sha256":"f8cd6055cf32e70a625e656db55163dc4a5300a3d83d81e3fb6a6f436f067c0d","abstract_canon_sha256":"8bcc40e17b72a869c20efac7ecb54268efc545458dfca8aba537836cbc309efc"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T03:15:37.865401Z","signature_b64":"jMXfRwKFRMV8VWk1qETS6h6z+KfpKDnTBuf3FVa16eUToAk+G8c/9NIMZmkB5Et9Su4gXlOEgelFRLdLiuZnBg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"7435b96acffd918985b91a3aa943d57d4b28fd9825762bad7be2aa36e2427131","last_reissued_at":"2026-07-05T03:15:37.864899Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T03:15:37.864899Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Long-term evolution of neutron-star merger remnants in general relativistic resistive-magnetohydrodynamics with a mean-field dynamo term","license":"http://creativecommons.org/licenses/by-nc-nd/4.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Masaru Shibata, Sho Fujibayashi, Yuichiro Sekiguchi","submitted_at":"2021-09-17T19:26:25Z","abstract_excerpt":"Long-term neutrino-radiation resistive-magnetohydrodynamics simulations in full general relativity are performed for a system composed of a massive neutron star and a torus formed as a remnant of binary neutron star mergers. The simulation is performed in axial symmetry incorporating a mean-field dynamo term for a hypothetical amplification of the magnetic-field strength. We first calibrate the mean-field dynamo parameters by comparing the results for the evolution of black hole-disk systems with viscous hydrodynamics results. We then perform simulations for the system of a remnant massive neu"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2109.08732","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":""},"integrity":{"clean":true,"summary":{"advisory":0,"critical":0,"by_detector":{},"informational":0},"endpoint":"/pith/2109.08732/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":"2109.08732","created_at":"2026-07-05T03:15:37.864952+00:00"},{"alias_kind":"arxiv_version","alias_value":"2109.08732v1","created_at":"2026-07-05T03:15:37.864952+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2109.08732","created_at":"2026-07-05T03:15:37.864952+00:00"},{"alias_kind":"pith_short_12","alias_value":"OQ23S2WP7WIY","created_at":"2026-07-05T03:15:37.864952+00:00"},{"alias_kind":"pith_short_16","alias_value":"OQ23S2WP7WIYTBNZ","created_at":"2026-07-05T03:15:37.864952+00:00"},{"alias_kind":"pith_short_8","alias_value":"OQ23S2WP","created_at":"2026-07-05T03:15:37.864952+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.12542","citing_title":"Implementation of multi-grid Poisson solver in numerical relativity and its application to gravitational collapse of massive star","ref_index":20,"is_internal_anchor":false},{"citing_arxiv_id":"2606.11299","citing_title":"A magnetar formation in binary neutron star merger","ref_index":120,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/OQ23S2WP7WIYTBNZDI5KSQ6VPV","json":"https://pith.science/pith/OQ23S2WP7WIYTBNZDI5KSQ6VPV.json","graph_json":"https://pith.science/api/pith-number/OQ23S2WP7WIYTBNZDI5KSQ6VPV/graph.json","events_json":"https://pith.science/api/pith-number/OQ23S2WP7WIYTBNZDI5KSQ6VPV/events.json","paper":"https://pith.science/paper/OQ23S2WP"},"agent_actions":{"view_html":"https://pith.science/pith/OQ23S2WP7WIYTBNZDI5KSQ6VPV","download_json":"https://pith.science/pith/OQ23S2WP7WIYTBNZDI5KSQ6VPV.json","view_paper":"https://pith.science/paper/OQ23S2WP","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2109.08732&json=true","fetch_graph":"https://pith.science/api/pith-number/OQ23S2WP7WIYTBNZDI5KSQ6VPV/graph.json","fetch_events":"https://pith.science/api/pith-number/OQ23S2WP7WIYTBNZDI5KSQ6VPV/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/OQ23S2WP7WIYTBNZDI5KSQ6VPV/action/timestamp_anchor","attest_storage":"https://pith.science/pith/OQ23S2WP7WIYTBNZDI5KSQ6VPV/action/storage_attestation","attest_author":"https://pith.science/pith/OQ23S2WP7WIYTBNZDI5KSQ6VPV/action/author_attestation","sign_citation":"https://pith.science/pith/OQ23S2WP7WIYTBNZDI5KSQ6VPV/action/citation_signature","submit_replication":"https://pith.science/pith/OQ23S2WP7WIYTBNZDI5KSQ6VPV/action/replication_record"}},"created_at":"2026-07-05T03:15:37.864952+00:00","updated_at":"2026-07-05T03:15:37.864952+00:00"}