Enomoto, RNaito, TTanimori, TYoshida, TYanagita, SMori, MasakiEdwards, Philip GAsahara, ABicknell, GeoffreyGunji, SHara, ShinjiHara, THayashi, SeiItoh, ChieKabuki, SKajino, FKatagiri, HKataoka, JKawachi, AKifune, TadashiKubo, HKushida, JMaeda, SMaeshiro, AMatsubara, YMizumoto, YMoriya, MieMuraishi, HMuraki, YNakase, TNishijima, KOhishi, MOkumora, KPatterson, Joseph RSakurazawa, KSuzuki, RSwaby, D LTakano, KTakata, MTokanai, FTsuchiya, KTsunoo, HUruma, KWatanabe, OYoshikoshi, T2015-12-130028-0836http://hdl.handle.net/1885/74615Protons with energies up to ∼1015 eV are the main component of cosmic rays, but evidence for the specific locations where they could have been accelerated to these energies has been lacking. Electrons are known to be accelerated to cosmic-ray energies iKeywords: Acceleration; Cosmic rays; Electrons; Gamma rays; Shock waves; Spectrum analysis; Upper atmosphere; Cosmic-ray protons; Protons; proton; cosmic ray; article; astronomy; cosmic radiation; electron; gamma radiation; negative pion radiation; photon; priority200210.1038/416823a2015-12-11