{"record_type":"pith_number_record","schema_url":"https://pith.science/schemas/pith-number/v1.json","pith_number":"pith:2004:OFKFRUS3DS3L7L6XX64CNKT7YO","short_pith_number":"pith:OFKFRUS3","schema_version":"1.0","canonical_sha256":"715458d25b1cb6bfafd7bfb826aa7fc3a28a0fcdd7df4b3d0dd5a2307da1492c","source":{"kind":"arxiv","id":"astro-ph/0405262","version":1},"attestation_state":"computed","paper":{"title":"The Physics of Neutron Stars","license":"","headline":"","cross_cats":["nucl-th"],"primary_cat":"astro-ph","authors_text":"J.M. Lattimer, M. Prakash","submitted_at":"2004-05-13T17:54:43Z","abstract_excerpt":"Neutron stars are some of the densest manifestations of massive objects in the universe. They are ideal astrophysical laboratories for testing theories of dense matter physics and provide connections among nuclear physics, particle physics and astrophysics. Neutron stars may exhibit conditions and phenomena not observed elsewhere, such as hyperon-dominated matter, deconfined quark matter, superfluidity and superconductivity with critical temperatures near ${10^{10}}$ kelvin, opaqueness to neutrinos, and magnetic fields in excess of $10^{13}$ Gauss. Here, we describe the formation, structure, i"},"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":"astro-ph/0405262","kind":"arxiv","version":1},"metadata":{"license":"","primary_cat":"astro-ph","submitted_at":"2004-05-13T17:54:43Z","cross_cats_sorted":["nucl-th"],"title_canon_sha256":"8d34523a3a719ecb247f93c2018e6c844e533362f8157937332db3df917024bd","abstract_canon_sha256":"43fc177e846ecf601e43ea3022390ae8b9fb232f3b0c95c82e6c7a4e5ed82d37"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-05-18T04:23:00.739766Z","signature_b64":"yzznPLxK2Kr10Q5mHcqoLvj/TMGbI/Kfjg1swyOn7iJo7m1GH07DC3aVXM0eCbr9PPpt9gkHslZ/h+CobiWcDg==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"715458d25b1cb6bfafd7bfb826aa7fc3a28a0fcdd7df4b3d0dd5a2307da1492c","last_reissued_at":"2026-05-18T04:23:00.739039Z","signature_status":"signed_v1","first_computed_at":"2026-05-18T04:23:00.739039Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"The Physics of Neutron Stars","license":"","headline":"","cross_cats":["nucl-th"],"primary_cat":"astro-ph","authors_text":"J.M. Lattimer, M. Prakash","submitted_at":"2004-05-13T17:54:43Z","abstract_excerpt":"Neutron stars are some of the densest manifestations of massive objects in the universe. They are ideal astrophysical laboratories for testing theories of dense matter physics and provide connections among nuclear physics, particle physics and astrophysics. Neutron stars may exhibit conditions and phenomena not observed elsewhere, such as hyperon-dominated matter, deconfined quark matter, superfluidity and superconductivity with critical temperatures near ${10^{10}}$ kelvin, opaqueness to neutrinos, and magnetic fields in excess of $10^{13}$ Gauss. Here, we describe the formation, structure, i"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0405262","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":"astro-ph/0405262","created_at":"2026-05-18T04:23:00.739164+00:00"},{"alias_kind":"arxiv_version","alias_value":"astro-ph/0405262v1","created_at":"2026-05-18T04:23:00.739164+00:00"},{"alias_kind":"doi","alias_value":"10.48550/arxiv.astro-ph/0405262","created_at":"2026-05-18T04:23:00.739164+00:00"},{"alias_kind":"pith_short_12","alias_value":"OFKFRUS3DS3L","created_at":"2026-05-18T12:25:52.687210+00:00"},{"alias_kind":"pith_short_16","alias_value":"OFKFRUS3DS3L7L6X","created_at":"2026-05-18T12:25:52.687210+00:00"},{"alias_kind":"pith_short_8","alias_value":"OFKFRUS3","created_at":"2026-05-18T12:25:52.687210+00:00"}],"events":[],"event_summary":{},"paper_claims":[],"inbound_citations":{"count":6,"internal_anchor_count":3,"sample":[{"citing_arxiv_id":"2509.04028","citing_title":"Primordial black holes versus their impersonators at gravitational wave observatories","ref_index":70,"is_internal_anchor":true},{"citing_arxiv_id":"2512.24194","citing_title":"Impact of Anisotropy on Neutron Star Structure and Curvature","ref_index":12,"is_internal_anchor":true},{"citing_arxiv_id":"2603.01061","citing_title":"QCD phase transition at finite isospin density and magnetic field","ref_index":19,"is_internal_anchor":true},{"citing_arxiv_id":"2604.02782","citing_title":"Spin effects in superfluidity, neutron matter and neutron stars","ref_index":5,"is_internal_anchor":false},{"citing_arxiv_id":"2604.20159","citing_title":"A Poincar\\'e-covariant study of strange quark stars","ref_index":15,"is_internal_anchor":false},{"citing_arxiv_id":"2605.02467","citing_title":"Modeling large glitches with core superfluidity in a Hybrid star","ref_index":3,"is_internal_anchor":false}]},"formal_canon":{"evidence_count":0,"sample":[],"anchors":[]},"links":{"html":"https://pith.science/pith/OFKFRUS3DS3L7L6XX64CNKT7YO","json":"https://pith.science/pith/OFKFRUS3DS3L7L6XX64CNKT7YO.json","graph_json":"https://pith.science/api/pith-number/OFKFRUS3DS3L7L6XX64CNKT7YO/graph.json","events_json":"https://pith.science/api/pith-number/OFKFRUS3DS3L7L6XX64CNKT7YO/events.json","paper":"https://pith.science/paper/OFKFRUS3"},"agent_actions":{"view_html":"https://pith.science/pith/OFKFRUS3DS3L7L6XX64CNKT7YO","download_json":"https://pith.science/pith/OFKFRUS3DS3L7L6XX64CNKT7YO.json","view_paper":"https://pith.science/paper/OFKFRUS3","resolve_alias":"https://pith.science/api/pith-number/resolve?arxiv=astro-ph/0405262&json=true","fetch_graph":"https://pith.science/api/pith-number/OFKFRUS3DS3L7L6XX64CNKT7YO/graph.json","fetch_events":"https://pith.science/api/pith-number/OFKFRUS3DS3L7L6XX64CNKT7YO/events.json","actions":{"anchor_timestamp":"https://pith.science/pith/OFKFRUS3DS3L7L6XX64CNKT7YO/action/timestamp_anchor","attest_storage":"https://pith.science/pith/OFKFRUS3DS3L7L6XX64CNKT7YO/action/storage_attestation","attest_author":"https://pith.science/pith/OFKFRUS3DS3L7L6XX64CNKT7YO/action/author_attestation","sign_citation":"https://pith.science/pith/OFKFRUS3DS3L7L6XX64CNKT7YO/action/citation_signature","submit_replication":"https://pith.science/pith/OFKFRUS3DS3L7L6XX64CNKT7YO/action/replication_record"}},"created_at":"2026-05-18T04:23:00.739164+00:00","updated_at":"2026-05-18T04:23:00.739164+00:00"}