{"record":{"author":{"account_ref":null,"orcid":null},"builds_on":[],"content_schema":"pubphys.content.topic/1","content_sha256":"e7916a3927ebd6cb6318deced21be25e21f6716e2a4e7a4945938927ff959848","created":"2026-10-03T07:17:52Z","files":[],"origin":{"assisted_by":[],"kind":"seed"},"parents":[],"salt":"39088d0ada0919f0a08c4ba87739b638aa4fbd10befe71735ea16eb712ff1154","schema":"pubphys.record/2","site":"pubphys.com","target":null,"type":"topic"},"content":{"external_id":"plasma.reconnection","field":"plasma","n":"1","review_cite":"H. Ji, J. Yoo, W. Fox, M. Yamada et al., Laboratory Study of Collisionless Magnetic Reconnection, arXiv:2307.07109, 2023","review_link":"https://arxiv.org/abs/2307.07109","review_verified":"true","summary":"Magnetic field lines in a plasma can break and rejoin, suddenly turning stored magnetic energy into heat, fast flows and very energetic particles. Simple theory says this should be far too slow to power solar flares, yet in nature it happens fast.","title":"Fast magnetic reconnection and particle energization","topic_ref":null,"why":"Reconnection powers solar flares, magnetospheric substorms, sawtooth crashes in tokamaks and probably the brightest high-energy astrophysical flares."},"attested":{"attestation":{"batch":null,"client_id":null,"id_token_sha256":null,"kind":"platform"},"record_hash":"c1057caf785ec309864fe9c3911636cf72981d9ad70fccb8c56b4c4d20d44a4f","schema":"pubphys.attested/1"},"envelope":{"attested_hash":"b0f28e8140422ae33ebaffe8787080e04793bc07c46b358c00716420e37de4ca","platform_signature":{"key_id":"c6afc19b31429869751f06879c75cd64ea92654423d15b44be775bf1310a60da","sig":"HpM-8h9Tc4wenVMcqdwd5TCdrCGQwYwsYkWhAApaBo9o8H4lqnYHDwCP9crXnp5T_D7fBvLMny8EEJknGsFlAA"},"schema":"pubphys.envelope/1"},"record_hash":"c1057caf785ec309864fe9c3911636cf72981d9ad70fccb8c56b4c4d20d44a4f","leaf_index":305}