{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:XGBS73HTOADOW5OAIZRIFYKE24","short_pith_number":"pith:XGBS73HT","schema_version":"1.0","canonical_sha256":"b9832fecf37006eb75c0466282e144d73dfede0b2d9af5994a6bc686fa2119cc","source":{"kind":"arxiv","id":"2502.14962","version":2},"attestation_state":"computed","paper":{"title":"Long-term impact of the magnetic-field strength on the evolution and electromagnetic emission by neutron-star merger remnants","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.HE","authors_text":"Harry Ho-Yin Ng, Jin-Liang Jiang, Luciano Rezzolla, Michail Chabanov","submitted_at":"2025-02-20T19:00:11Z","abstract_excerpt":"Numerical simulations are essential to understand the complex physics accompanying the merger of binary systems of neutron stars. However, these simulations become computationally challenging when they have to model the merger remnants on timescales over which secular phenomena, such as the launching of magnetically driven outflows, develop. To tackle these challenges, we have recently developed a hybrid approach that combines, via a hand-off transition, a fully general-relativistic code (FIL) with a more efficient code making use of the conformally flat approximation (BHAC+). We here report i"},"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":"2502.14962","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.HE","submitted_at":"2025-02-20T19:00:11Z","cross_cats_sorted":["gr-qc"],"title_canon_sha256":"1dbbcec904a52f465fa836171d1daeedfc4705cf4b7295ee1bacaec131028bc6","abstract_canon_sha256":"68aacd46a22168903fdc4e09618e53cf40bdd2fef23cdf2f57f4caaac3f9cb24"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T11:18:18.319553Z","signature_b64":"2R/+wcXFelm2Oq11otTVo/UyQL3CWKN8AYd/wvD2RGre0pEkbsdpEjC1Jkg2Ti79vOD/HSKfavGt1yaFbpd9Cg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"b9832fecf37006eb75c0466282e144d73dfede0b2d9af5994a6bc686fa2119cc","last_reissued_at":"2026-07-05T11:18:18.319043Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T11:18:18.319043Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Long-term impact of the magnetic-field strength on the evolution and electromagnetic emission by neutron-star merger remnants","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.HE","authors_text":"Harry Ho-Yin Ng, Jin-Liang Jiang, Luciano Rezzolla, Michail Chabanov","submitted_at":"2025-02-20T19:00:11Z","abstract_excerpt":"Numerical simulations are essential to understand the complex physics accompanying the merger of binary systems of neutron stars. However, these simulations become computationally challenging when they have to model the merger remnants on timescales over which secular phenomena, such as the launching of magnetically driven outflows, develop. To tackle these challenges, we have recently developed a hybrid approach that combines, via a hand-off transition, a fully general-relativistic code (FIL) with a more efficient code making use of the conformally flat approximation (BHAC+). We here report i"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2502.14962","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/2502.14962/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":"2502.14962","created_at":"2026-07-05T11:18:18.319103+00:00"},{"alias_kind":"arxiv_version","alias_value":"2502.14962v2","created_at":"2026-07-05T11:18:18.319103+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2502.14962","created_at":"2026-07-05T11:18:18.319103+00:00"},{"alias_kind":"pith_short_12","alias_value":"XGBS73HTOADO","created_at":"2026-07-05T11:18:18.319103+00:00"},{"alias_kind":"pith_short_16","alias_value":"XGBS73HTOADOW5OA","created_at":"2026-07-05T11:18:18.319103+00:00"},{"alias_kind":"pith_short_8","alias_value":"XGBS73HT","created_at":"2026-07-05T11:18:18.319103+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2605.03947","citing_title":"Effects of magnetically driven shocks on nucleosynthesis and kilonovae from neutron star mergers","ref_index":37,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/XGBS73HTOADOW5OAIZRIFYKE24","json":"https://pith.science/pith/XGBS73HTOADOW5OAIZRIFYKE24.json","graph_json":"https://pith.science/api/pith-number/XGBS73HTOADOW5OAIZRIFYKE24/graph.json","events_json":"https://pith.science/api/pith-number/XGBS73HTOADOW5OAIZRIFYKE24/events.json","paper":"https://pith.science/paper/XGBS73HT"},"agent_actions":{"view_html":"https://pith.science/pith/XGBS73HTOADOW5OAIZRIFYKE24","download_json":"https://pith.science/pith/XGBS73HTOADOW5OAIZRIFYKE24.json","view_paper":"https://pith.science/paper/XGBS73HT","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2502.14962&json=true","fetch_graph":"https://pith.science/api/pith-number/XGBS73HTOADOW5OAIZRIFYKE24/graph.json","fetch_events":"https://pith.science/api/pith-number/XGBS73HTOADOW5OAIZRIFYKE24/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/XGBS73HTOADOW5OAIZRIFYKE24/action/timestamp_anchor","attest_storage":"https://pith.science/pith/XGBS73HTOADOW5OAIZRIFYKE24/action/storage_attestation","attest_author":"https://pith.science/pith/XGBS73HTOADOW5OAIZRIFYKE24/action/author_attestation","sign_citation":"https://pith.science/pith/XGBS73HTOADOW5OAIZRIFYKE24/action/citation_signature","submit_replication":"https://pith.science/pith/XGBS73HTOADOW5OAIZRIFYKE24/action/replication_record"}},"created_at":"2026-07-05T11:18:18.319103+00:00","updated_at":"2026-07-05T11:18:18.319103+00:00"}