{"record":{"author":{"account_ref":null,"orcid":null},"builds_on":[],"content_schema":"pubphys.content.topic/1","content_sha256":"5d3feec7bd9e383f573965e4283de8c7b1e22b529136c0b93b548ba906c17a19","created":"2026-10-03T07:17:51Z","files":[],"origin":{"assisted_by":[],"kind":"seed"},"parents":[],"salt":"3dd0c63cf35395c871870000d5f907ede5944df920a6a03fb7785c3994079e8b","schema":"pubphys.record/2","site":"pubphys.com","target":null,"type":"topic"},"content":{"external_id":"grav.bh-microstates","field":"grav","n":"1","review_cite":"A. Strominger, C. Vafa, Microscopic origin of the Bekenstein-Hawking entropy, Phys. Lett. B 379, 99, 1996","review_link":"https://arxiv.org/abs/hep-th/9601029","review_verified":"true","summary":"A black hole has an entropy equal to a quarter of its horizon area in Planck units, which means it has an enormous number of hidden internal states. String theory counts these states exactly for special charged, zero-temperature black holes, but not for ordinary ones.","title":"Microscopic origin of non-extremal black hole entropy","topic_ref":null,"why":"Counting the states of an ordinary black hole would identify the microscopic degrees of freedom of quantum gravity."},"attested":{"attestation":{"batch":null,"client_id":null,"id_token_sha256":null,"kind":"platform"},"record_hash":"1035ad33d8a9ccd80488cee2f65c345c1f7222bd089aa039ccbbf4731a2f59f2","schema":"pubphys.attested/1"},"envelope":{"attested_hash":"f14ca9b31640e7f463c010b151cb7f7ddc4555e59b1a9d5f1a997c2160ae6573","platform_signature":{"key_id":"c6afc19b31429869751f06879c75cd64ea92654423d15b44be775bf1310a60da","sig":"RjE3HXGxkvxM2aX-fv7BPMAEAQmesx3SxzpYlohXYrUyFteA1r2yAteWa_Z0Dy0NzLesIX7sUJjvRVemyrWlCw"},"schema":"pubphys.envelope/1"},"record_hash":"1035ad33d8a9ccd80488cee2f65c345c1f7222bd089aa039ccbbf4731a2f59f2","leaf_index":228}