{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2025:ANNXGY6OVG3ITI4N4WWMZ3C6JS","short_pith_number":"pith:ANNXGY6O","schema_version":"1.0","canonical_sha256":"035b7363cea9b689a38de5acccec5e4c945a7970e4b9deffa2680712d1cba48b","source":{"kind":"arxiv","id":"2503.17445","version":1},"attestation_state":"computed","paper":{"title":"$^{56}$Ni production in long-lived binary neutron star merger remnants","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Albino Perego, Almudena Arcones, Eleonora Loffredo, Fabio Magistrelli, Giacomo Ricigliano, Leonardo Chiesa, Maximilian Jacobi, Sebastiano Bernuzzi","submitted_at":"2025-03-21T18:00:00Z","abstract_excerpt":"We investigate the nucleosynthesis and kilonova emission based on numerical-relativity binary neutron star merger simulations that incorporate a two-moment neutrino-transport scheme. Unlike in previous works with simpler neutrino treatments, a massive, fast (up to $v=0.3c$), proton-rich neutrino-driven wind develops in the post-merger phase of the simulations as long as the merger remnant does not collapse to a black hole. We evolve the ejecta for 100 days after the merger using 2D ray-by-ray radiation-hydrodynamics simulations coupled in-situ to a complete nuclear network. The most abundant n"},"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":"2503.17445","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.HE","submitted_at":"2025-03-21T18:00:00Z","cross_cats_sorted":[],"title_canon_sha256":"26f9ed4c6afd83862def15cd97465a1740dab5285c1a43e6fbd22e1690997720","abstract_canon_sha256":"94e5d97700e88b5dc6cfb798ede414d69afd86b5962434eeaad2116365e9eb8f"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T10:37:09.464052Z","signature_b64":"3TnMbhYUUSG6xHeqzUkk2DzPUPRr0Sc//BMfcyCdHlA59tyi+Sr0VfpogmD020D+de/w+JoJs14wEFV8HwzXBQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"035b7363cea9b689a38de5acccec5e4c945a7970e4b9deffa2680712d1cba48b","last_reissued_at":"2026-07-05T10:37:09.463525Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T10:37:09.463525Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"$^{56}$Ni production in long-lived binary neutron star merger remnants","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":[],"primary_cat":"astro-ph.HE","authors_text":"Albino Perego, Almudena Arcones, Eleonora Loffredo, Fabio Magistrelli, Giacomo Ricigliano, Leonardo Chiesa, Maximilian Jacobi, Sebastiano Bernuzzi","submitted_at":"2025-03-21T18:00:00Z","abstract_excerpt":"We investigate the nucleosynthesis and kilonova emission based on numerical-relativity binary neutron star merger simulations that incorporate a two-moment neutrino-transport scheme. Unlike in previous works with simpler neutrino treatments, a massive, fast (up to $v=0.3c$), proton-rich neutrino-driven wind develops in the post-merger phase of the simulations as long as the merger remnant does not collapse to a black hole. We evolve the ejecta for 100 days after the merger using 2D ray-by-ray radiation-hydrodynamics simulations coupled in-situ to a complete nuclear network. The most abundant n"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2503.17445","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/2503.17445/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":"2503.17445","created_at":"2026-07-05T10:37:09.463579+00:00"},{"alias_kind":"arxiv_version","alias_value":"2503.17445v1","created_at":"2026-07-05T10:37:09.463579+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2503.17445","created_at":"2026-07-05T10:37:09.463579+00:00"},{"alias_kind":"pith_short_12","alias_value":"ANNXGY6OVG3I","created_at":"2026-07-05T10:37:09.463579+00:00"},{"alias_kind":"pith_short_16","alias_value":"ANNXGY6OVG3ITI4N","created_at":"2026-07-05T10:37:09.463579+00:00"},{"alias_kind":"pith_short_8","alias_value":"ANNXGY6O","created_at":"2026-07-05T10:37:09.463579+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":3,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.11299","citing_title":"A magnetar formation in binary neutron star merger","ref_index":61,"is_internal_anchor":false},{"citing_arxiv_id":"2512.11032","citing_title":"Impact of in situ nuclear networks and atomic opacities on neutron star merger ejecta dynamics, nucleosynthesis, and kilonovae","ref_index":44,"is_internal_anchor":false},{"citing_arxiv_id":"2603.08792","citing_title":"Gamma-ray Signatures of r-Process Radioactivity from the Collapse of Magnetized White Dwarfs","ref_index":54,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/ANNXGY6OVG3ITI4N4WWMZ3C6JS","json":"https://pith.science/pith/ANNXGY6OVG3ITI4N4WWMZ3C6JS.json","graph_json":"https://pith.science/api/pith-number/ANNXGY6OVG3ITI4N4WWMZ3C6JS/graph.json","events_json":"https://pith.science/api/pith-number/ANNXGY6OVG3ITI4N4WWMZ3C6JS/events.json","paper":"https://pith.science/paper/ANNXGY6O"},"agent_actions":{"view_html":"https://pith.science/pith/ANNXGY6OVG3ITI4N4WWMZ3C6JS","download_json":"https://pith.science/pith/ANNXGY6OVG3ITI4N4WWMZ3C6JS.json","view_paper":"https://pith.science/paper/ANNXGY6O","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2503.17445&json=true","fetch_graph":"https://pith.science/api/pith-number/ANNXGY6OVG3ITI4N4WWMZ3C6JS/graph.json","fetch_events":"https://pith.science/api/pith-number/ANNXGY6OVG3ITI4N4WWMZ3C6JS/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/ANNXGY6OVG3ITI4N4WWMZ3C6JS/action/timestamp_anchor","attest_storage":"https://pith.science/pith/ANNXGY6OVG3ITI4N4WWMZ3C6JS/action/storage_attestation","attest_author":"https://pith.science/pith/ANNXGY6OVG3ITI4N4WWMZ3C6JS/action/author_attestation","sign_citation":"https://pith.science/pith/ANNXGY6OVG3ITI4N4WWMZ3C6JS/action/citation_signature","submit_replication":"https://pith.science/pith/ANNXGY6OVG3ITI4N4WWMZ3C6JS/action/replication_record"}},"created_at":"2026-07-05T10:37:09.463579+00:00","updated_at":"2026-07-05T10:37:09.463579+00:00"}