{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2020:QWUXEMFJ4POZT44PRNK6UAJN5L","short_pith_number":"pith:QWUXEMFJ","schema_version":"1.0","canonical_sha256":"85a97230a9e3dd99f38f8b55ea012deacec4f4ef5cdd8bd22ae2852307c74ff4","source":{"kind":"arxiv","id":"2007.10424","version":2},"attestation_state":"computed","paper":{"title":"Thermodynamical Description of Hot, Rapidly Rotating Neutron Stars, Protoneutron Stars, and Neutron Star Merger Remnants","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["gr-qc","nucl-th"],"primary_cat":"astro-ph.HE","authors_text":"Ch.C. Moustakidis, P.S. Koliogiannis","submitted_at":"2020-07-20T19:28:45Z","abstract_excerpt":"The prediction of the equation of state of hot, dense nuclear matter is one of the most complicated and interesting problems in nuclear astrophysics. At the same time, knowledge of it is the basic ingredient for some of the most interesting studies. In the present work, we concentrate our study on the construction of the equation of state of hot, dense nuclear matter, related mainly to the interior of the neutron star. We employ a theoretical nuclear model, which includes momentum-dependent interaction among the nucleons, along with the \\textit{state-of-the-art} microscopic calculations. Therm"},"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":"2007.10424","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"astro-ph.HE","submitted_at":"2020-07-20T19:28:45Z","cross_cats_sorted":["gr-qc","nucl-th"],"title_canon_sha256":"9d0c9ccd118e0117ead99c0c526c80cef16d60759125fb1cf4741336318664a8","abstract_canon_sha256":"832d7d10fb66b515f8054dba6f09aa5048c2a27a1cbadb5b8d01ae524d8dbc4a"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T02:39:03.380415Z","signature_b64":"AnXNKSt2Xje4C+olH+whiyBLLiFkURf+KYw9WBdZgMLOmZNaHEw80BPo4OKYEn4fFJCuODYPbU43d7khaea/CA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"85a97230a9e3dd99f38f8b55ea012deacec4f4ef5cdd8bd22ae2852307c74ff4","last_reissued_at":"2026-07-05T02:39:03.379924Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T02:39:03.379924Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Thermodynamical Description of Hot, Rapidly Rotating Neutron Stars, Protoneutron Stars, and Neutron Star Merger Remnants","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["gr-qc","nucl-th"],"primary_cat":"astro-ph.HE","authors_text":"Ch.C. Moustakidis, P.S. Koliogiannis","submitted_at":"2020-07-20T19:28:45Z","abstract_excerpt":"The prediction of the equation of state of hot, dense nuclear matter is one of the most complicated and interesting problems in nuclear astrophysics. At the same time, knowledge of it is the basic ingredient for some of the most interesting studies. In the present work, we concentrate our study on the construction of the equation of state of hot, dense nuclear matter, related mainly to the interior of the neutron star. We employ a theoretical nuclear model, which includes momentum-dependent interaction among the nucleons, along with the \\textit{state-of-the-art} microscopic calculations. Therm"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2007.10424","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/2007.10424/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":"2007.10424","created_at":"2026-07-05T02:39:03.379980+00:00"},{"alias_kind":"arxiv_version","alias_value":"2007.10424v2","created_at":"2026-07-05T02:39:03.379980+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2007.10424","created_at":"2026-07-05T02:39:03.379980+00:00"},{"alias_kind":"pith_short_12","alias_value":"QWUXEMFJ4POZ","created_at":"2026-07-05T02:39:03.379980+00:00"},{"alias_kind":"pith_short_16","alias_value":"QWUXEMFJ4POZT44P","created_at":"2026-07-05T02:39:03.379980+00:00"},{"alias_kind":"pith_short_8","alias_value":"QWUXEMFJ","created_at":"2026-07-05T02:39:03.379980+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2412.07758","citing_title":"Fastest spinning millisecond pulsars: indicators for quark matter in neutron stars?","ref_index":96,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/QWUXEMFJ4POZT44PRNK6UAJN5L","json":"https://pith.science/pith/QWUXEMFJ4POZT44PRNK6UAJN5L.json","graph_json":"https://pith.science/api/pith-number/QWUXEMFJ4POZT44PRNK6UAJN5L/graph.json","events_json":"https://pith.science/api/pith-number/QWUXEMFJ4POZT44PRNK6UAJN5L/events.json","paper":"https://pith.science/paper/QWUXEMFJ"},"agent_actions":{"view_html":"https://pith.science/pith/QWUXEMFJ4POZT44PRNK6UAJN5L","download_json":"https://pith.science/pith/QWUXEMFJ4POZT44PRNK6UAJN5L.json","view_paper":"https://pith.science/paper/QWUXEMFJ","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2007.10424&json=true","fetch_graph":"https://pith.science/api/pith-number/QWUXEMFJ4POZT44PRNK6UAJN5L/graph.json","fetch_events":"https://pith.science/api/pith-number/QWUXEMFJ4POZT44PRNK6UAJN5L/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/QWUXEMFJ4POZT44PRNK6UAJN5L/action/timestamp_anchor","attest_storage":"https://pith.science/pith/QWUXEMFJ4POZT44PRNK6UAJN5L/action/storage_attestation","attest_author":"https://pith.science/pith/QWUXEMFJ4POZT44PRNK6UAJN5L/action/author_attestation","sign_citation":"https://pith.science/pith/QWUXEMFJ4POZT44PRNK6UAJN5L/action/citation_signature","submit_replication":"https://pith.science/pith/QWUXEMFJ4POZT44PRNK6UAJN5L/action/replication_record"}},"created_at":"2026-07-05T02:39:03.379980+00:00","updated_at":"2026-07-05T02:39:03.379980+00:00"}