{"paper":{"title":"Cooling of Akmal-Pandharipande-Ravenhall neutron star models","license":"","headline":"","cross_cats":[],"primary_cat":"astro-ph","authors_text":"(2) Ohio State Univ.), A.D. Kaminker (1), D.G. Yakovlev (1), M.E. Gusakov (1), O.Y. Gnedin (2) ((1) Ioffe Institute","submitted_at":"2005-07-23T13:17:17Z","abstract_excerpt":"We study the cooling of superfluid neutron stars whose cores consist of nucleon matter with the Akmal-Pandharipande-Ravenhall equation of state. This equation of state opens the powerful direct Urca process of neutrino emission in the interior of most massive neutron stars. Extending our previous studies (Gusakov et al. 2004a, Kaminker et al. 2005), we employ phenomenological density-dependent critical temperatures T_{cp}(\\rho) of strong singlet-state proton pairing (with the maximum T_{cp}^{max} \\sim 7e9 K in the outer stellar core) and T_{cnt}(\\rho) of moderate triplet-state neutron pairing "},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"astro-ph/0507560","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"}