{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2021:734BNQK53ZO7W4Y2N6ERGK3D4G","short_pith_number":"pith:734BNQK5","schema_version":"1.0","canonical_sha256":"fef816c15dde5dfb731a6f89132b63e18288f3571ea308f005a712f7fbd39acd","source":{"kind":"arxiv","id":"2105.03747","version":1},"attestation_state":"computed","paper":{"title":"Neutron Stars and the Nuclear Equation of State","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"nucl-th","authors_text":"G. F. Burgio, H.-J. Schulze, I. Vidana, J.-B. Wei (INFN Sezione di Catania)","submitted_at":"2021-05-08T17:25:09Z","abstract_excerpt":"We review the current status and recent progress of microscopic many-body approaches and phenomenological models, which are employed to construct the equation of state of neutron stars. The equation of state is relevant for the description of their structure and dynamical properties, and it rules also the dynamics of core-collapse supernovae and binary neutron star mergers. We describe neutron star matter assuming that the main degrees of freedom are nucleons and hyperons, disregarding the appearance of quark matter. We compare the theoretical predictions of the different equation-of-state mod"},"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":"2105.03747","kind":"arxiv","version":1},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"nucl-th","submitted_at":"2021-05-08T17:25:09Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"d4091cacfd37b063429b19af6ce2644af6fbcee0b1ae4499d9990f94cdab0f24","abstract_canon_sha256":"0a83631ead631fd81da4df3912785affc167b80b28d01c8dd04918893c7c9f3f"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T03:23:41.203690Z","signature_b64":"maBK0g/sY45029a2jybRPshkQ8pEOdyY92NBgalo9etKFBUNZ471Nlk//h3BmwKeT0M561t5kbUN9w4r0yXwDQ==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"fef816c15dde5dfb731a6f89132b63e18288f3571ea308f005a712f7fbd39acd","last_reissued_at":"2026-07-05T03:23:41.203109Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T03:23:41.203109Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Neutron Stars and the Nuclear Equation of State","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"nucl-th","authors_text":"G. F. Burgio, H.-J. Schulze, I. Vidana, J.-B. Wei (INFN Sezione di Catania)","submitted_at":"2021-05-08T17:25:09Z","abstract_excerpt":"We review the current status and recent progress of microscopic many-body approaches and phenomenological models, which are employed to construct the equation of state of neutron stars. The equation of state is relevant for the description of their structure and dynamical properties, and it rules also the dynamics of core-collapse supernovae and binary neutron star mergers. We describe neutron star matter assuming that the main degrees of freedom are nucleons and hyperons, disregarding the appearance of quark matter. We compare the theoretical predictions of the different equation-of-state mod"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2105.03747","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/2105.03747/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":"2105.03747","created_at":"2026-07-05T03:23:41.203163+00:00"},{"alias_kind":"arxiv_version","alias_value":"2105.03747v1","created_at":"2026-07-05T03:23:41.203163+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2105.03747","created_at":"2026-07-05T03:23:41.203163+00:00"},{"alias_kind":"pith_short_12","alias_value":"734BNQK53ZO7","created_at":"2026-07-05T03:23:41.203163+00:00"},{"alias_kind":"pith_short_16","alias_value":"734BNQK53ZO7W4Y2","created_at":"2026-07-05T03:23:41.203163+00:00"},{"alias_kind":"pith_short_8","alias_value":"734BNQK5","created_at":"2026-07-05T03:23:41.203163+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":12,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.21435","citing_title":"Is the coexistence of strange quark stars and hadronic stars favored by astrophysical data? A Bayesian analysis","ref_index":1,"is_internal_anchor":false},{"citing_arxiv_id":"2606.20957","citing_title":"Out-of-Equilibrium Effects in Non-Radial Relativistic Stellar Perturbations: A Model-Agnostic Formulation and Mode Analysis","ref_index":22,"is_internal_anchor":false},{"citing_arxiv_id":"2606.19446","citing_title":"Dynamical Tidal Response of Neutron Stars: from Effective Field Theory to Gravitational Waveforms","ref_index":4,"is_internal_anchor":false},{"citing_arxiv_id":"2606.02690","citing_title":"Speed and accuracy for long signals: Frequency-domain effective-one-body waveforms for compact binary coalescences","ref_index":33,"is_internal_anchor":false},{"citing_arxiv_id":"2606.31389","citing_title":"Cooling of Hybrid Stars with a 2SC+$<dd>$ Phase","ref_index":20,"is_internal_anchor":false},{"citing_arxiv_id":"2606.29510","citing_title":"Radial oscillations of quark stars in light of current astrophysical constraints: A comparative study","ref_index":10,"is_internal_anchor":false},{"citing_arxiv_id":"2605.26658","citing_title":"Isospin-breaking effects on the threshold cusp structures in $\\Lambda N$-$\\Sigma N$ scattering","ref_index":26,"is_internal_anchor":false},{"citing_arxiv_id":"2507.15951","citing_title":"Distinguishing Neutron Star vs. Low-Mass Black Hole Binaries with Late Inspiral & Postmerger Gravitational Waves $-$ Sensitivity to Transmuted Black Holes and Non-Annihilating Dark Matter","ref_index":69,"is_internal_anchor":false},{"citing_arxiv_id":"2605.09723","citing_title":"Cooling of Isolated Neutron Stars with Hyperon-mixed Kaon-Condensation Matter","ref_index":10,"is_internal_anchor":false},{"citing_arxiv_id":"2604.18214","citing_title":"Collision Energy Dependence of Hypertriton Production in Au+Au Collisions at RHIC","ref_index":6,"is_internal_anchor":false},{"citing_arxiv_id":"2604.07949","citing_title":"Wave-Function Femtometry: Hypertriton - The Ultimate Halo Nucleus","ref_index":4,"is_internal_anchor":false},{"citing_arxiv_id":"2605.07745","citing_title":"The massive Thirring / sine-Gordon model with non-zero current density","ref_index":9,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/734BNQK53ZO7W4Y2N6ERGK3D4G","json":"https://pith.science/pith/734BNQK53ZO7W4Y2N6ERGK3D4G.json","graph_json":"https://pith.science/api/pith-number/734BNQK53ZO7W4Y2N6ERGK3D4G/graph.json","events_json":"https://pith.science/api/pith-number/734BNQK53ZO7W4Y2N6ERGK3D4G/events.json","paper":"https://pith.science/paper/734BNQK5"},"agent_actions":{"view_html":"https://pith.science/pith/734BNQK53ZO7W4Y2N6ERGK3D4G","download_json":"https://pith.science/pith/734BNQK53ZO7W4Y2N6ERGK3D4G.json","view_paper":"https://pith.science/paper/734BNQK5","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2105.03747&json=true","fetch_graph":"https://pith.science/api/pith-number/734BNQK53ZO7W4Y2N6ERGK3D4G/graph.json","fetch_events":"https://pith.science/api/pith-number/734BNQK53ZO7W4Y2N6ERGK3D4G/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/734BNQK53ZO7W4Y2N6ERGK3D4G/action/timestamp_anchor","attest_storage":"https://pith.science/pith/734BNQK53ZO7W4Y2N6ERGK3D4G/action/storage_attestation","attest_author":"https://pith.science/pith/734BNQK53ZO7W4Y2N6ERGK3D4G/action/author_attestation","sign_citation":"https://pith.science/pith/734BNQK53ZO7W4Y2N6ERGK3D4G/action/citation_signature","submit_replication":"https://pith.science/pith/734BNQK53ZO7W4Y2N6ERGK3D4G/action/replication_record"}},"created_at":"2026-07-05T03:23:41.203163+00:00","updated_at":"2026-07-05T03:23:41.203163+00:00"}