{"record":{"author":{"account_ref":null,"orcid":null},"builds_on":[],"content_schema":"pubphys.content.topic/1","content_sha256":"9fb5bcd5fc11f46fbe2d950e1589a48077858eb93fe18a684e7843f908ca79dd","created":"2026-10-03T07:17:52Z","files":[],"origin":{"assisted_by":[],"kind":"seed"},"parents":[],"salt":"bec3e453531aa4b046c7935e6148b0b0e5a514c763f822d45814cbed782d568b","schema":"pubphys.record/2","site":"pubphys.com","target":null,"type":"topic"},"content":{"external_id":"nuc.stellar-reaction-rates","field":"nuc","n":"1","review_cite":"R. J. deBoer, J. Gorres, M. Wiescher et al., The 12C(alpha,gamma)16O reaction and its implications for stellar helium burning, Reviews of Modern Physics, 2017","review_link":"https://doi.org/10.1103/RevModPhys.89.035007","review_verified":"true","summary":"Stars make elements through nuclear reactions at energies so low that the reactions are too rare to measure directly in the laboratory, so their rates must be extrapolated. Some elements, such as certain molybdenum and ruthenium isotopes or the products of a medium-speed neutron-capture process, still have no confirmed stellar origin.","title":"Stellar reaction rates and non-r-process nucleosynthesis","topic_ref":null,"why":"The rates set how stars burn, how they die, and which elements they leave behind, so errors in them propagate into every model of stellar evolution and galactic chemistry."},"attested":{"attestation":{"batch":null,"client_id":null,"id_token_sha256":null,"kind":"platform"},"record_hash":"a34c6b5ed7af37b4290d97a2613b13b71248636c2138e338345ab4d03e765618","schema":"pubphys.attested/1"},"envelope":{"attested_hash":"4cc7eaf93b3727cad0724895e5d8dcb7eb6740afae681c5bb26ceabe0d6b18f2","platform_signature":{"key_id":"c6afc19b31429869751f06879c75cd64ea92654423d15b44be775bf1310a60da","sig":"q0pE16gZJOCwmN-6uHguGRxGIoU3RYSfpoKxLVY7PELs_j_7dDwnvS1DcHtHKpWsITlE011n-Ivhpydypp_HAg"},"schema":"pubphys.envelope/1"},"record_hash":"a34c6b5ed7af37b4290d97a2613b13b71248636c2138e338345ab4d03e765618","leaf_index":295}