{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2018:HMJ6TZS4ELNNTESI52Z64O54YD","short_pith_number":"pith:HMJ6TZS4","schema_version":"1.0","canonical_sha256":"3b13e9e65c22dad99248eeb3ee3bbcc0e17f903bf0c497b768f68fac4fb5b4ef","source":{"kind":"arxiv","id":"1810.10992","version":2},"attestation_state":"computed","paper":{"title":"Predicting the moment of inertia of pulsar J0737-3039A from Bayesian modeling of 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":"Jeremy W. Holt, Robert J. Stahulak, Yeunhwan Lim","submitted_at":"2018-10-25T17:34:05Z","abstract_excerpt":"We investigate neutron star moments of inertia from Bayesian posterior probability distributions of the nuclear equation of state that incorporate information from microscopic many-body theory and empirical data of finite nuclei. We focus on PSR J0737-3039A and predict that for this 1.338 M_sun neutron star the moment of inertia lies in the range $1.04 \\times 10^{45}$ g cm$^{2} < I < 1.51 \\times 10^{45}$ g cm$^{2}$ at the 95% credibility level, while the most probable value for the moment of inertia is $\\tilde I = 1.36 \\times 10^{45}$ g cm$^{2}$. Assuming a measurement of the PSR J0737-3039A 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":"1810.10992","kind":"arxiv","version":2},"metadata":{"license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","primary_cat":"nucl-th","submitted_at":"2018-10-25T17:34:05Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"e623db5731c953353e818f3c4d803129fe3a153328e4d6dc195c97db0f24ba9f","abstract_canon_sha256":"8f9a3dbaa5a1be81e4836a92996c56a936658b411d4abb8534ac2a73fd9f45ba"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T00:04:38.447424Z","signature_b64":"4Egx/e65fZeE4Z8kh/s1MHdH9/98Z0PrA25vVeNWcGQceOtpauvZr1UdIP+f3VWaY3cNQ15hoHOCXtjao1KRBA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"3b13e9e65c22dad99248eeb3ee3bbcc0e17f903bf0c497b768f68fac4fb5b4ef","last_reissued_at":"2026-07-05T00:04:38.446948Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T00:04:38.446948Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Predicting the moment of inertia of pulsar J0737-3039A from Bayesian modeling of 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":"Jeremy W. Holt, Robert J. Stahulak, Yeunhwan Lim","submitted_at":"2018-10-25T17:34:05Z","abstract_excerpt":"We investigate neutron star moments of inertia from Bayesian posterior probability distributions of the nuclear equation of state that incorporate information from microscopic many-body theory and empirical data of finite nuclei. We focus on PSR J0737-3039A and predict that for this 1.338 M_sun neutron star the moment of inertia lies in the range $1.04 \\times 10^{45}$ g cm$^{2} < I < 1.51 \\times 10^{45}$ g cm$^{2}$ at the 95% credibility level, while the most probable value for the moment of inertia is $\\tilde I = 1.36 \\times 10^{45}$ g cm$^{2}$. Assuming a measurement of the PSR J0737-3039A m"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1810.10992","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/1810.10992/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":"1810.10992","created_at":"2026-07-05T00:04:38.447007+00:00"},{"alias_kind":"arxiv_version","alias_value":"1810.10992v2","created_at":"2026-07-05T00:04:38.447007+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.1810.10992","created_at":"2026-07-05T00:04:38.447007+00:00"},{"alias_kind":"pith_short_12","alias_value":"HMJ6TZS4ELNN","created_at":"2026-07-05T00:04:38.447007+00:00"},{"alias_kind":"pith_short_16","alias_value":"HMJ6TZS4ELNNTESI","created_at":"2026-07-05T00:04:38.447007+00:00"},{"alias_kind":"pith_short_8","alias_value":"HMJ6TZS4","created_at":"2026-07-05T00:04:38.447007+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":1,"internal_anchor_count":1,"sample":[{"citing_arxiv_id":"2502.07902","citing_title":"Building Neutron Stars with the MUSES Calculation Engine","ref_index":89,"is_internal_anchor":true}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/HMJ6TZS4ELNNTESI52Z64O54YD","json":"https://pith.science/pith/HMJ6TZS4ELNNTESI52Z64O54YD.json","graph_json":"https://pith.science/api/pith-number/HMJ6TZS4ELNNTESI52Z64O54YD/graph.json","events_json":"https://pith.science/api/pith-number/HMJ6TZS4ELNNTESI52Z64O54YD/events.json","paper":"https://pith.science/paper/HMJ6TZS4"},"agent_actions":{"view_html":"https://pith.science/pith/HMJ6TZS4ELNNTESI52Z64O54YD","download_json":"https://pith.science/pith/HMJ6TZS4ELNNTESI52Z64O54YD.json","view_paper":"https://pith.science/paper/HMJ6TZS4","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=1810.10992&json=true","fetch_graph":"https://pith.science/api/pith-number/HMJ6TZS4ELNNTESI52Z64O54YD/graph.json","fetch_events":"https://pith.science/api/pith-number/HMJ6TZS4ELNNTESI52Z64O54YD/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/HMJ6TZS4ELNNTESI52Z64O54YD/action/timestamp_anchor","attest_storage":"https://pith.science/pith/HMJ6TZS4ELNNTESI52Z64O54YD/action/storage_attestation","attest_author":"https://pith.science/pith/HMJ6TZS4ELNNTESI52Z64O54YD/action/author_attestation","sign_citation":"https://pith.science/pith/HMJ6TZS4ELNNTESI52Z64O54YD/action/citation_signature","submit_replication":"https://pith.science/pith/HMJ6TZS4ELNNTESI52Z64O54YD/action/replication_record"}},"created_at":"2026-07-05T00:04:38.447007+00:00","updated_at":"2026-07-05T00:04:38.447007+00:00"}