{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2012:ESDYMAY7SKLCEORJVFESOQRZK4","short_pith_number":"pith:ESDYMAY7","schema_version":"1.0","canonical_sha256":"248786031f9296223a29a9492742395733428b364b4a3db7811f00e23e943c6a","source":{"kind":"arxiv","id":"1207.2184","version":1},"attestation_state":"computed","paper":{"title":"Core-collapse supernova equations of state based on neutron star observations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["nucl-th"],"primary_cat":"astro-ph.SR","authors_text":"Andrew W. Steiner, Matthias Hempel, Tobias Fischer","submitted_at":"2012-07-09T21:00:43Z","abstract_excerpt":"Many of the currently available equations of state for core-collapse supernova simulations give large neutron star radii and do not provide large enough neutron star masses, both of which are inconsistent with some recent neutron star observations. In addition, one of the critical uncertainties in the nucleon-nucleon interaction, the nuclear symmetry energy, is not fully explored by the currently available equations of state. In this article, we construct two new equations of state which match recent neutron star observations and provide more flexibility in studying the dependence on nuclear m"},"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":"1207.2184","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"astro-ph.SR","submitted_at":"2012-07-09T21:00:43Z","cross_cats_sorted":["nucl-th"],"title_canon_sha256":"d5f17949900a80ec780c2c79b494ba9a5a5cd3c277894156dd0f8b833cf6a851","abstract_canon_sha256":"98f1062925193ae1b50ec4ddde2c7f6e5c74f65479707da55f9c79e4a8615361"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T01:56:26.193532Z","signature_b64":"f6VLX4JlDSp6BIRjAceCTJDfou8BghbxLNxiO3Hec7czySR9YlOfN4/rTewzT5LU7rpjiybL3BLjf51T8GwxBw==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"248786031f9296223a29a9492742395733428b364b4a3db7811f00e23e943c6a","last_reissued_at":"2026-05-18T01:56:26.192773Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T01:56:26.192773Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Core-collapse supernova equations of state based on neutron star observations","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["nucl-th"],"primary_cat":"astro-ph.SR","authors_text":"Andrew W. Steiner, Matthias Hempel, Tobias Fischer","submitted_at":"2012-07-09T21:00:43Z","abstract_excerpt":"Many of the currently available equations of state for core-collapse supernova simulations give large neutron star radii and do not provide large enough neutron star masses, both of which are inconsistent with some recent neutron star observations. In addition, one of the critical uncertainties in the nucleon-nucleon interaction, the nuclear symmetry energy, is not fully explored by the currently available equations of state. In this article, we construct two new equations of state which match recent neutron star observations and provide more flexibility in studying the dependence on nuclear m"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1207.2184","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":"1207.2184","created_at":"2026-05-18T01:56:26.192867+00:00"},{"alias_kind":"arxiv_version","alias_value":"1207.2184v1","created_at":"2026-05-18T01:56:26.192867+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1207.2184","created_at":"2026-05-18T01:56:26.192867+00:00"},{"alias_kind":"pith_short_12","alias_value":"ESDYMAY7SKLC","created_at":"2026-05-18T12:27:04.183437+00:00"},{"alias_kind":"pith_short_16","alias_value":"ESDYMAY7SKLCEORJ","created_at":"2026-05-18T12:27:04.183437+00:00"},{"alias_kind":"pith_short_8","alias_value":"ESDYMAY7","created_at":"2026-05-18T12:27:04.183437+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":9,"internal_anchor_count":6,"sample":[{"citing_arxiv_id":"2302.12089","citing_title":"Time integration for neutrino radiation transport using minimally implicit Runge-Kutta methods","ref_index":34,"is_internal_anchor":true},{"citing_arxiv_id":"2605.21578","citing_title":"Gravitational wave detectability range informed by external messengers","ref_index":42,"is_internal_anchor":true},{"citing_arxiv_id":"2605.16504","citing_title":"Neutrino Flavor Conversion Shapes the Rate of Failed Core-collapse Supernovae","ref_index":66,"is_internal_anchor":true},{"citing_arxiv_id":"2605.18972","citing_title":"Flavor Conversion Enhances or Suppresses Supernova Explodability Independent of the Progenitor Mass","ref_index":64,"is_internal_anchor":true},{"citing_arxiv_id":"2509.13322","citing_title":"Axion-photon conversion in transient compact stars: Systematics, constraints, and opportunities","ref_index":72,"is_internal_anchor":true},{"citing_arxiv_id":"2603.08843","citing_title":"Matter- and magnetically-driven flavor conversion of neutrinos in magnetorotational collapses","ref_index":55,"is_internal_anchor":true},{"citing_arxiv_id":"2605.03947","citing_title":"Effects of magnetically driven shocks on nucleosynthesis and kilonovae from neutron star mergers","ref_index":64,"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":108,"is_internal_anchor":false},{"citing_arxiv_id":"2604.06404","citing_title":"Neutrino transport and flavor instabilities in a post-merger disk","ref_index":104,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/ESDYMAY7SKLCEORJVFESOQRZK4","json":"https://pith.science/pith/ESDYMAY7SKLCEORJVFESOQRZK4.json","graph_json":"https://pith.science/api/pith-number/ESDYMAY7SKLCEORJVFESOQRZK4/graph.json","events_json":"https://pith.science/api/pith-number/ESDYMAY7SKLCEORJVFESOQRZK4/events.json","paper":"https://pith.science/paper/ESDYMAY7"},"agent_actions":{"view_html":"https://pith.science/pith/ESDYMAY7SKLCEORJVFESOQRZK4","download_json":"https://pith.science/pith/ESDYMAY7SKLCEORJVFESOQRZK4.json","view_paper":"https://pith.science/paper/ESDYMAY7","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1207.2184&json=true","fetch_graph":"https://pith.science/api/pith-number/ESDYMAY7SKLCEORJVFESOQRZK4/graph.json","fetch_events":"https://pith.science/api/pith-number/ESDYMAY7SKLCEORJVFESOQRZK4/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/ESDYMAY7SKLCEORJVFESOQRZK4/action/timestamp_anchor","attest_storage":"https://pith.science/pith/ESDYMAY7SKLCEORJVFESOQRZK4/action/storage_attestation","attest_author":"https://pith.science/pith/ESDYMAY7SKLCEORJVFESOQRZK4/action/author_attestation","sign_citation":"https://pith.science/pith/ESDYMAY7SKLCEORJVFESOQRZK4/action/citation_signature","submit_replication":"https://pith.science/pith/ESDYMAY7SKLCEORJVFESOQRZK4/action/replication_record"}},"created_at":"2026-05-18T01:56:26.192867+00:00","updated_at":"2026-05-18T01:56:26.192867+00:00"}