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We compute the rate of the Urca\n  process in compact stars taking into account the non-Fermi liquid\n  contributions to the proton's spectral widths induced by short-range\n  correlations. The Urca rate differs strongly from the Fermi-liquid\n  prediction at low temperatures, in particular, the h"},"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":"2406.16183","kind":"arxiv","version":3},"metadata":{"license":"http://creativecommons.org/licenses/by/4.0/","primary_cat":"nucl-th","submitted_at":"2024-06-23T18:22:56Z","cross_cats_sorted":["astro-ph.HE"],"title_canon_sha256":"3b0a974800e4e91fc589159d148c2492448f4b8df4fca969df17e22282e7970a","abstract_canon_sha256":"5cd8e27f3ff7a77e749b8802aafbc2345b014a944ef2450c933f1aa979313054"},"schema_version":"1.0"},"receipt":{"kind":"pith_receipt","key_id":"pith-v1-2026-05","algorithm":"ed25519","signed_at":"2026-07-05T09:25:44.731240Z","signature_b64":"ZJjnscYEduUfSN3GApndv5OHrI7oOKEK/enF9/tDTWuR/9DREpZXT6BdRp8qpkJZLwkSL+ZaOpyJTGZRFSg+CA==","signed_message":"canonical_sha256_bytes","builder_version":"pith-number-builder-2026-05-17-v1","receipt_version":"0.3","canonical_sha256":"010545508453c81f102a856f71455d3e178d3624e3a1474704f5bd6a512f7cf6","last_reissued_at":"2026-07-05T09:25:44.730715Z","signature_status":"signed_v1","first_computed_at":"2026-07-05T09:25:44.730715Z","public_key_fingerprint":"8d4b5ee74e4693bcd1df2446408b0d54"},"graph_snapshot":{"paper":{"title":"Short-Range Correlations and Urca Process in Neutron Stars","license":"http://creativecommons.org/licenses/by/4.0/","headline":"","cross_cats":["astro-ph.HE"],"primary_cat":"nucl-th","authors_text":"Armen Sedrakian","submitted_at":"2024-06-23T18:22:56Z","abstract_excerpt":"Recent measurements of high-momentum correlated neutron-proton pairs\n  at JLab suggest that the dense nucleonic component of the compact\n  stars contains a fraction of high-momentum neutron-proton pairs that\n  is not accounted for in the familiar Fermi-liquid theory of the\n  neutron-proton fluid mixture. We compute the rate of the Urca\n  process in compact stars taking into account the non-Fermi liquid\n  contributions to the proton's spectral widths induced by short-range\n  correlations. 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