{"record":{"author":{"account_ref":null,"orcid":null},"builds_on":[],"content_schema":"pubphys.content.topic/1","content_sha256":"71a24c42544e8f9506ecb92e1e7e1a0c0bbc43b367756772b80b59355c511edc","created":"2026-10-03T07:17:51Z","files":[],"origin":{"assisted_by":[],"kind":"seed"},"parents":[],"salt":"ce814532d7caa8f17be88c771c44c7be8cb8c3c8db8c5b6fd70ed2af5f8f1c40","schema":"pubphys.record/2","site":"pubphys.com","target":null,"type":"topic"},"content":{"external_id":"grav.evaporation-backreaction","field":"grav","n":"1","review_cite":"S. Hollands, R. M. Wald, Quantum fields in curved spacetime, Phys. Rep. 574, 1, 2015","review_link":"https://arxiv.org/abs/1401.2026","review_verified":"true","summary":"As a black hole radiates it loses mass and gets hotter, so evaporation speeds up toward a final burst. What is left at the end, and how the radiation reshapes spacetime along the way, requires quantum gravity or careful approximations.","title":"Black hole evaporation endpoint","topic_ref":null,"why":"The endpoint decides whether information is returned, stored, or lost."},"attested":{"attestation":{"batch":null,"client_id":null,"id_token_sha256":null,"kind":"platform"},"record_hash":"c6f0f7e9427ae2192894c5f52b801031bd05930fb85200c49b24b33d76d27ba6","schema":"pubphys.attested/1"},"envelope":{"attested_hash":"af1e1061e1ed6898249c7836c41ad14c34eb10dc48558418ff13ad9e4f602594","platform_signature":{"key_id":"c6afc19b31429869751f06879c75cd64ea92654423d15b44be775bf1310a60da","sig":"EEfD7h86IVtJEnxOGj0fWNRjE7pChgYY51jtoucJGaoEuD0u8W8LMcu3ZIUJwAJEFVH9nec3fGspO1bKcLrZDA"},"schema":"pubphys.envelope/1"},"record_hash":"c6f0f7e9427ae2192894c5f52b801031bd05930fb85200c49b24b33d76d27ba6","leaf_index":229}