{"record":{"author":{"account_ref":null,"orcid":null},"builds_on":[],"content_schema":"pubphys.content.topic/1","content_sha256":"1b998abf3b404696470931b6b4b5d4503d5990282712902078fde81d46f9b077","created":"2026-10-03T07:17:50Z","files":[],"origin":{"assisted_by":[],"kind":"seed"},"parents":[],"salt":"0d77c8a13827649ec1f98ee84b007bdcdb07306eeb9b8aa1199aded121caf7d4","schema":"pubphys.record/2","site":"pubphys.com","target":null,"type":"topic"},"content":{"external_id":"astro.neutron-star-interiors","field":"astro","n":"1","review_cite":"B. Haskell, A. Melatos, Models of Pulsar Glitches, International Journal of Modern Physics D, 2015","review_link":"https://arxiv.org/abs/1502.07062","review_verified":"true","summary":"Neutron stars are city-size balls of neutrons whose interiors are expected to be superfluid, a frictionless quantum liquid. Sudden spin-ups called glitches, the cooling of young stars and the absence of certain gravitational waves test that picture.","title":"Neutron-star glitches, superfluidity and cooling","topic_ref":null,"why":"These observations are the main laboratory for nuclear superfluidity at densities that no experiment on Earth can reach."},"attested":{"attestation":{"batch":null,"client_id":null,"id_token_sha256":null,"kind":"platform"},"record_hash":"afd1feb0d7ec84994296c83f9c2ecba96e22fc9ddf5d5fa7c0562e1f6f4eb1d4","schema":"pubphys.attested/1"},"envelope":{"attested_hash":"cfba32af2286320c72df5091f44f32b6aa02104a055caa9293854f7c9c0ac649","platform_signature":{"key_id":"c6afc19b31429869751f06879c75cd64ea92654423d15b44be775bf1310a60da","sig":"K5XPqdcmBdupN6rWRPR6IDquJszm-m9js3fLq92XvMDmBUiBZmxFqBe_Gwlu2yNnjVisPSkA3Yq9lLmFaVEQCw"},"schema":"pubphys.envelope/1"},"record_hash":"afd1feb0d7ec84994296c83f9c2ecba96e22fc9ddf5d5fa7c0562e1f6f4eb1d4","leaf_index":45}