{"record":{"author":{"account_ref":null,"orcid":null},"builds_on":[],"content_schema":"pubphys.content.topic/1","content_sha256":"16c845dcff04184f6ed935c5a3a718a9ceb078698bc7128490b1f48a5aa890cf","created":"2026-10-03T07:17:52Z","files":[],"origin":{"assisted_by":[],"kind":"seed"},"parents":[],"salt":"c130e433a6c04262ec39d8b212f31855573ceb47174c81fda4dc883b5cd5d412","schema":"pubphys.record/2","site":"pubphys.com","target":null,"type":"topic"},"content":{"external_id":"plasma.kinetic-turbulence-dynamo","field":"plasma","n":"1","review_cite":"D. Verscharen, K. G. Klein, B. A. Maruca, The multi-scale nature of the solar wind, Living Reviews in Solar Physics, 2019","review_link":"https://arxiv.org/abs/1902.03448","review_verified":"true","summary":"The solar wind is a hot, nearly collision-free plasma that stays much hotter than simple expansion predicts, so its turbulence must heat it, but without collisions it is unclear how the energy becomes heat. In similar plasmas, turbulent motion can amplify weak magnetic fields (a dynamo), and how that works without collisions is also open.","title":"Collisionless turbulence, heating and plasma dynamos","topic_ref":null,"why":"These processes set the temperatures of the solar wind, galaxy-cluster gas and black-hole accretion flows, and the origin of cosmic magnetic fields."},"attested":{"attestation":{"batch":null,"client_id":null,"id_token_sha256":null,"kind":"platform"},"record_hash":"0fbe23e43e59314b73b802e78f2d2325c4a6b8b6a539d5dd3f6690b91375cb5f","schema":"pubphys.attested/1"},"envelope":{"attested_hash":"5a5ca1de64e83556ecc2cf513644cb70d56aae2b7bbb91527a70dfed71d2ee4b","platform_signature":{"key_id":"c6afc19b31429869751f06879c75cd64ea92654423d15b44be775bf1310a60da","sig":"2QgFOWA9-VHjoZA9RuJyldy7lQTeUHnAHwzrW3ZuINcEvyyZyIMJ7CdxYdTPZpErMSk9oB--1Z4T8dUuezd7DA"},"schema":"pubphys.envelope/1"},"record_hash":"0fbe23e43e59314b73b802e78f2d2325c4a6b8b6a539d5dd3f6690b91375cb5f","leaf_index":302}