{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2024:EUUN677EG2TMCLI7HV6ECFP7IF","short_pith_number":"pith:EUUN677E","schema_version":"1.0","canonical_sha256":"2528df7fe436a6c12d1f3d7c4115ff417220376581c846bd32f5f8934c0dc473","source":{"kind":"arxiv","id":"2412.05923","version":2},"attestation_state":"computed","paper":{"title":"Implications of latest NICER data for the neutron star equation of state","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.HE","gr-qc","nucl-ex"],"primary_cat":"nucl-th","authors_text":"Len Brandes, Wolfram Weise","submitted_at":"2024-12-08T12:37:29Z","abstract_excerpt":"As an update to our previously performed Bayesian inference analyses of the neutron star matter equation-of-state and related quantities, the additional impact of the recently published NICER data of PSR J0437-4751 is examined. Including the mass and radius distributions of this pulsar in our data base results in modest shifts from previously inferred median posterior values of radii $R$ and central densities $n_c$ for representative $1.4\\,M_\\odot$ and $2.1\\,M_\\odot$ neutron stars: radii are reduced by about $0.2-0.3$ km to values of $R_{1.4} = 12.1\\pm 0.5$ km and $R_{2.1} = 11.9^{+0.5}_{-0.6}"},"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":"2412.05923","kind":"arxiv","version":2},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"nucl-th","submitted_at":"2024-12-08T12:37:29Z","cross_cats_sorted":["astro-ph.HE","gr-qc","nucl-ex"],"title_canon_sha256":"cf587b6d3f835e68f8550432b34cfb09b484ca7b46583a2be090295f4124efac","abstract_canon_sha256":"26d415332cc1bf92e8899f1789cf9332ec44c5e157daadaae1f10a35851bbf18"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T10:27:21.333834Z","signature_b64":"myORl7Qy/gjNvFm6mgKNHtHbhanRtyNWRhO3paV/xi/RYUHd8HpHT30EwTU9V+2AGWsyin8CD1AJUXPh2exKAA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"2528df7fe436a6c12d1f3d7c4115ff417220376581c846bd32f5f8934c0dc473","last_reissued_at":"2026-07-05T10:27:21.333368Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T10:27:21.333368Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Implications of latest NICER data for the neutron star equation of state","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.HE","gr-qc","nucl-ex"],"primary_cat":"nucl-th","authors_text":"Len Brandes, Wolfram Weise","submitted_at":"2024-12-08T12:37:29Z","abstract_excerpt":"As an update to our previously performed Bayesian inference analyses of the neutron star matter equation-of-state and related quantities, the additional impact of the recently published NICER data of PSR J0437-4751 is examined. Including the mass and radius distributions of this pulsar in our data base results in modest shifts from previously inferred median posterior values of radii $R$ and central densities $n_c$ for representative $1.4\\,M_\\odot$ and $2.1\\,M_\\odot$ neutron stars: radii are reduced by about $0.2-0.3$ km to values of $R_{1.4} = 12.1\\pm 0.5$ km and $R_{2.1} = 11.9^{+0.5}_{-0.6}"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"2412.05923","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/2412.05923/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":"2412.05923","created_at":"2026-07-05T10:27:21.333428+00:00"},{"alias_kind":"arxiv_version","alias_value":"2412.05923v2","created_at":"2026-07-05T10:27:21.333428+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.2412.05923","created_at":"2026-07-05T10:27:21.333428+00:00"},{"alias_kind":"pith_short_12","alias_value":"EUUN677EG2TM","created_at":"2026-07-05T10:27:21.333428+00:00"},{"alias_kind":"pith_short_16","alias_value":"EUUN677EG2TMCLI7","created_at":"2026-07-05T10:27:21.333428+00:00"},{"alias_kind":"pith_short_8","alias_value":"EUUN677E","created_at":"2026-07-05T10:27:21.333428+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":2,"internal_anchor_count":0,"sample":[{"citing_arxiv_id":"2606.02966","citing_title":"Sensitivity of the Neutron Star Equation of State Inferences to Mass and Radius Measurements","ref_index":18,"is_internal_anchor":false},{"citing_arxiv_id":"2512.24194","citing_title":"Impact of Anisotropy on Neutron Star Structure and Curvature","ref_index":7,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/EUUN677EG2TMCLI7HV6ECFP7IF","json":"https://pith.science/pith/EUUN677EG2TMCLI7HV6ECFP7IF.json","graph_json":"https://pith.science/api/pith-number/EUUN677EG2TMCLI7HV6ECFP7IF/graph.json","events_json":"https://pith.science/api/pith-number/EUUN677EG2TMCLI7HV6ECFP7IF/events.json","paper":"https://pith.science/paper/EUUN677E"},"agent_actions":{"view_html":"https://pith.science/pith/EUUN677EG2TMCLI7HV6ECFP7IF","download_json":"https://pith.science/pith/EUUN677EG2TMCLI7HV6ECFP7IF.json","view_paper":"https://pith.science/paper/EUUN677E","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=2412.05923&json=true","fetch_graph":"https://pith.science/api/pith-number/EUUN677EG2TMCLI7HV6ECFP7IF/graph.json","fetch_events":"https://pith.science/api/pith-number/EUUN677EG2TMCLI7HV6ECFP7IF/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/EUUN677EG2TMCLI7HV6ECFP7IF/action/timestamp_anchor","attest_storage":"https://pith.science/pith/EUUN677EG2TMCLI7HV6ECFP7IF/action/storage_attestation","attest_author":"https://pith.science/pith/EUUN677EG2TMCLI7HV6ECFP7IF/action/author_attestation","sign_citation":"https://pith.science/pith/EUUN677EG2TMCLI7HV6ECFP7IF/action/citation_signature","submit_replication":"https://pith.science/pith/EUUN677EG2TMCLI7HV6ECFP7IF/action/replication_record"}},"created_at":"2026-07-05T10:27:21.333428+00:00","updated_at":"2026-07-05T10:27:21.333428+00:00"}