{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2022:IER3XSXKPLRJABT45WP4XBOF3H","short_pith_number":"pith:IER3XSXK","schema_version":"1.0","canonical_sha256":"4123bbcaea7ae290067ced9fcb85c5d9ce81a2016a32ad727309746dad90b48e","source":{"kind":"arxiv","id":"2209.02538","version":2},"attestation_state":"computed","paper":{"title":"Neutrino transport in general relativistic neutron star merger simulations","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.HE","authors_text":"Francois Foucart","submitted_at":"2022-09-06T14:39:21Z","abstract_excerpt":"Numerical simulations of neutron star--neutron star and neutron star--black hole binaries play an important role in our ability to model gravitational wave and electromagnetic signals powered by these systems. These simulations have to take into account a wide range of physical processes including general relativity, magnetohydrodynamics, and neutrino radiation transport. The latter is particularly important in order to understand the properties of the matter ejected by many mergers, the optical/infrared signals powered by nuclear reactions in the ejecta, and the contribution of that ejecta to"},"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":"2209.02538","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.HE","submitted_at":"2022-09-06T14:39:21Z","cross_cats_sorted":["gr-qc"],"title_canon_sha256":"c26fc78d2834eabd3c55840fe942a585a6af3573a177e9ed1ed0b9fd1f73548c","abstract_canon_sha256":"77f4dec53061b7b2fce7bfb1ba920413a55f83dcaae085dca451fdbcb148a8b2"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T05:51:41.669620Z","signature_b64":"QDdZsfvHldbyUiq/0A1l0KxIfgwB28tu/MCeFySU4tL4KUbbq/NOjm3R58bXzjNVyAAY1nVdC/QFVdPrY8ysDw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"4123bbcaea7ae290067ced9fcb85c5d9ce81a2016a32ad727309746dad90b48e","last_reissued_at":"2026-07-05T05:51:41.669166Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T05:51:41.669166Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Neutrino transport in general relativistic neutron star merger simulations","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["gr-qc"],"primary_cat":"astro-ph.HE","authors_text":"Francois Foucart","submitted_at":"2022-09-06T14:39:21Z","abstract_excerpt":"Numerical simulations of neutron star--neutron star and neutron star--black hole binaries play an important role in our ability to model gravitational wave and electromagnetic signals powered by these systems. These simulations have to take into account a wide range of physical processes including general relativity, magnetohydrodynamics, and neutrino radiation transport. The latter is particularly important in order to understand the properties of the matter ejected by many mergers, the optical/infrared signals powered by nuclear reactions in the ejecta, and the contribution of that ejecta to"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2209.02538","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/2209.02538/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":"2209.02538","created_at":"2026-07-05T05:51:41.669223+00:00"},{"alias_kind":"arxiv_version","alias_value":"2209.02538v2","created_at":"2026-07-05T05:51:41.669223+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2209.02538","created_at":"2026-07-05T05:51:41.669223+00:00"},{"alias_kind":"pith_short_12","alias_value":"IER3XSXKPLRJ","created_at":"2026-07-05T05:51:41.669223+00:00"},{"alias_kind":"pith_short_16","alias_value":"IER3XSXKPLRJABT4","created_at":"2026-07-05T05:51:41.669223+00:00"},{"alias_kind":"pith_short_8","alias_value":"IER3XSXK","created_at":"2026-07-05T05:51:41.669223+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":6,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.12404","citing_title":"Collective neutrino oscillations: Many-body non-forward effects and non-classicality","ref_index":12,"is_internal_anchor":false},{"citing_arxiv_id":"2605.31242","citing_title":"Neutrino helicity oscillations in astrophysical environments: a many-body approach","ref_index":18,"is_internal_anchor":false},{"citing_arxiv_id":"2606.27425","citing_title":"Impact of neutrino-electron scattering and an improved treatment of pair processes on binary neutron star mergers","ref_index":14,"is_internal_anchor":false},{"citing_arxiv_id":"2605.29187","citing_title":"Assessing the Relative Importance of Neutrino Matter Interaction Channels in Post-Merger Remnant of Binary Neutron Stars","ref_index":67,"is_internal_anchor":false},{"citing_arxiv_id":"2410.20681","citing_title":"Influence of neutrino-electron scattering and neutrino-pair annihilation on hypermassive neutron star","ref_index":32,"is_internal_anchor":false},{"citing_arxiv_id":"2509.25838","citing_title":"Bulk viscosity from neutron decays to dark baryons in neutron star matter","ref_index":88,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/IER3XSXKPLRJABT45WP4XBOF3H","json":"https://pith.science/pith/IER3XSXKPLRJABT45WP4XBOF3H.json","graph_json":"https://pith.science/api/pith-number/IER3XSXKPLRJABT45WP4XBOF3H/graph.json","events_json":"https://pith.science/api/pith-number/IER3XSXKPLRJABT45WP4XBOF3H/events.json","paper":"https://pith.science/paper/IER3XSXK"},"agent_actions":{"view_html":"https://pith.science/pith/IER3XSXKPLRJABT45WP4XBOF3H","download_json":"https://pith.science/pith/IER3XSXKPLRJABT45WP4XBOF3H.json","view_paper":"https://pith.science/paper/IER3XSXK","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2209.02538&json=true","fetch_graph":"https://pith.science/api/pith-number/IER3XSXKPLRJABT45WP4XBOF3H/graph.json","fetch_events":"https://pith.science/api/pith-number/IER3XSXKPLRJABT45WP4XBOF3H/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/IER3XSXKPLRJABT45WP4XBOF3H/action/timestamp_anchor","attest_storage":"https://pith.science/pith/IER3XSXKPLRJABT45WP4XBOF3H/action/storage_attestation","attest_author":"https://pith.science/pith/IER3XSXKPLRJABT45WP4XBOF3H/action/author_attestation","sign_citation":"https://pith.science/pith/IER3XSXKPLRJABT45WP4XBOF3H/action/citation_signature","submit_replication":"https://pith.science/pith/IER3XSXKPLRJABT45WP4XBOF3H/action/replication_record"}},"created_at":"2026-07-05T05:51:41.669223+00:00","updated_at":"2026-07-05T05:51:41.669223+00:00"}