{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2009:ELO5VMWQEZCHAXH47OK6NK3DUQ","short_pith_number":"pith:ELO5VMWQ","schema_version":"1.0","canonical_sha256":"22dddab2d02644705cfcfb95e6ab63a43df9bd6ebc5e6f7048169bad05920efd","source":{"kind":"arxiv","id":"0911.4073","version":1},"attestation_state":"computed","paper":{"title":"Statistical Model for a Complete Supernova Equation of State","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"nucl-th","authors_text":"J\\\"urgen Schaffner-Bielich, Matthias Hempel","submitted_at":"2009-11-20T18:41:34Z","abstract_excerpt":"A statistical model for the equation of state (EOS) and the composition of supernova matter is presented with focus on the liquid-gas phase transition of nuclear matter. It consists of an ensemble of nuclei and interacting nucleons in nuclear statistical equilibrium. A relativistic mean field model is applied for the nucleons. The masses of the nuclei are taken from nuclear structure calculations which are based on the same nuclear Lagrangian. For known nuclei experimental data is used directly. Excluded volume effects are implemented in a thermodynamic consistent way so that the transition 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":"0911.4073","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"nucl-th","submitted_at":"2009-11-20T18:41:34Z","cross_cats_sorted":["astro-ph.SR"],"title_canon_sha256":"e61095c5fcc060eaf1aa5ec9cf4c01614bf55e66ee63e598cc979511d0cdce19","abstract_canon_sha256":"0608c27e5320578d58dcf9f98fcd0dfff67d7eb502eb5f7419b3136b9830c708"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T03:40:03.796694Z","signature_b64":"TVwXw0ZDBcdZgJUK7szxMwmjzi49jrJQ+5QZrLr1PMTBCampab7WnbbDLNjG4caPpUybJSgkgugIRw8X+ZzwBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"22dddab2d02644705cfcfb95e6ab63a43df9bd6ebc5e6f7048169bad05920efd","last_reissued_at":"2026-05-18T03:40:03.796207Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T03:40:03.796207Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Statistical Model for a Complete Supernova Equation of State","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.SR"],"primary_cat":"nucl-th","authors_text":"J\\\"urgen Schaffner-Bielich, Matthias Hempel","submitted_at":"2009-11-20T18:41:34Z","abstract_excerpt":"A statistical model for the equation of state (EOS) and the composition of supernova matter is presented with focus on the liquid-gas phase transition of nuclear matter. It consists of an ensemble of nuclei and interacting nucleons in nuclear statistical equilibrium. A relativistic mean field model is applied for the nucleons. The masses of the nuclei are taken from nuclear structure calculations which are based on the same nuclear Lagrangian. For known nuclei experimental data is used directly. Excluded volume effects are implemented in a thermodynamic consistent way so that the transition to"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"0911.4073","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":"0911.4073","created_at":"2026-05-18T03:40:03.796285+00:00"},{"alias_kind":"arxiv_version","alias_value":"0911.4073v1","created_at":"2026-05-18T03:40:03.796285+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.0911.4073","created_at":"2026-05-18T03:40:03.796285+00:00"},{"alias_kind":"pith_short_12","alias_value":"ELO5VMWQEZCH","created_at":"2026-05-18T12:25:59.703012+00:00"},{"alias_kind":"pith_short_16","alias_value":"ELO5VMWQEZCHAXH4","created_at":"2026-05-18T12:25:59.703012+00:00"},{"alias_kind":"pith_short_8","alias_value":"ELO5VMWQ","created_at":"2026-05-18T12:25:59.703012+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":7,"internal_anchor_count":4,"sample":[{"citing_arxiv_id":"2410.20681","citing_title":"Influence of neutrino-electron scattering and neutrino-pair annihilation on hypermassive neutron star","ref_index":37,"is_internal_anchor":true},{"citing_arxiv_id":"2605.21578","citing_title":"Gravitational wave detectability range informed by external messengers","ref_index":41,"is_internal_anchor":true},{"citing_arxiv_id":"2510.08707","citing_title":"Neutrino diagnostics of hadron-quark phase transition in Neutron Stars","ref_index":30,"is_internal_anchor":true},{"citing_arxiv_id":"2605.17563","citing_title":"Charged-current neutrino opacity within the relativistic Hartree-Fock framework for astrophysical simulations of core-collapse supernovae and binary neutron star mergers","ref_index":56,"is_internal_anchor":true},{"citing_arxiv_id":"2604.23503","citing_title":"Hyperaccreting Neutron Stars inside Massive Envelopes: The Implausibility of Thorne-\\.Zytkow Objects","ref_index":39,"is_internal_anchor":false},{"citing_arxiv_id":"2605.04896","citing_title":"Parameter Estimation Horizon of Core-Collapse Supernovae with Current and Next-Generation Gravitational-Wave Detectors","ref_index":110,"is_internal_anchor":false},{"citing_arxiv_id":"2604.11431","citing_title":"Impact of Effective Nucleon Mass and Multineutron States on the Equation of State for Core-Collapse Supernovae","ref_index":13,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/ELO5VMWQEZCHAXH47OK6NK3DUQ","json":"https://pith.science/pith/ELO5VMWQEZCHAXH47OK6NK3DUQ.json","graph_json":"https://pith.science/api/pith-number/ELO5VMWQEZCHAXH47OK6NK3DUQ/graph.json","events_json":"https://pith.science/api/pith-number/ELO5VMWQEZCHAXH47OK6NK3DUQ/events.json","paper":"https://pith.science/paper/ELO5VMWQ"},"agent_actions":{"view_html":"https://pith.science/pith/ELO5VMWQEZCHAXH47OK6NK3DUQ","download_json":"https://pith.science/pith/ELO5VMWQEZCHAXH47OK6NK3DUQ.json","view_paper":"https://pith.science/paper/ELO5VMWQ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=0911.4073&json=true","fetch_graph":"https://pith.science/api/pith-number/ELO5VMWQEZCHAXH47OK6NK3DUQ/graph.json","fetch_events":"https://pith.science/api/pith-number/ELO5VMWQEZCHAXH47OK6NK3DUQ/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/ELO5VMWQEZCHAXH47OK6NK3DUQ/action/timestamp_anchor","attest_storage":"https://pith.science/pith/ELO5VMWQEZCHAXH47OK6NK3DUQ/action/storage_attestation","attest_author":"https://pith.science/pith/ELO5VMWQEZCHAXH47OK6NK3DUQ/action/author_attestation","sign_citation":"https://pith.science/pith/ELO5VMWQEZCHAXH47OK6NK3DUQ/action/citation_signature","submit_replication":"https://pith.science/pith/ELO5VMWQEZCHAXH47OK6NK3DUQ/action/replication_record"}},"created_at":"2026-05-18T03:40:03.796285+00:00","updated_at":"2026-05-18T03:40:03.796285+00:00"}