{"record":{"author":{"account_ref":null,"orcid":null},"builds_on":[],"content_schema":"pubphys.content.topic/1","content_sha256":"44861d7c68c5b6bc639346c108942c14e1f351528c34cd380b36f8ec77d4bea0","created":"2026-10-03T07:17:51Z","files":[],"origin":{"assisted_by":[],"kind":"seed"},"parents":[],"salt":"f8eb889b14681a7cc35da93b9587406ff6b3791e6731bee91b45b811a49323f2","schema":"pubphys.record/2","site":"pubphys.com","target":null,"type":"topic"},"content":{"external_id":"grav.kerr-stability","field":"grav","n":"1","review_cite":"S. Klainerman, J. Szeftel, Kerr stability for small angular momentum, arXiv:2104.11857, 2021","review_link":"https://arxiv.org/abs/2104.11857","review_verified":"true","summary":"The Kerr solution describes a spinning black hole in Einstein's theory. To be the endpoint of real collapses it must be the only settled black hole and must be stable: when slightly disturbed, it should settle back to another Kerr black hole.","title":"Stability and uniqueness of Kerr black holes","topic_ref":null,"why":"Stability and uniqueness underpin the use of Kerr black holes as the final state of every astrophysical merger and of every ringdown test."},"attested":{"attestation":{"batch":null,"client_id":null,"id_token_sha256":null,"kind":"platform"},"record_hash":"be2aa7f5f2ad85604c5d4874af362613267361a54ca383af83a420f7d1ef76b3","schema":"pubphys.attested/1"},"envelope":{"attested_hash":"89ad2ad6589297a95f0f7522ed51b42157103d5a042dbd2e99dbb2f7ae8c40d3","platform_signature":{"key_id":"c6afc19b31429869751f06879c75cd64ea92654423d15b44be775bf1310a60da","sig":"t1K2lbtfheTmqPlATLkAyuImIMCo_3aZ1QklZjKqmL8WPfGHTDVBRM1q8mtfTYdBIrY2ZiACh5iPD09NYU3_Cw"},"schema":"pubphys.envelope/1"},"record_hash":"be2aa7f5f2ad85604c5d4874af362613267361a54ca383af83a420f7d1ef76b3","leaf_index":230}