ino ▁flux ▁above ▁a ▁minimum ▁energy . ▁The ▁det ector ▁S NO ▁used ▁scatter ing ▁on ▁de uter ium ▁that ▁allowed ▁to ▁measure ▁the ▁energy ▁of ▁the ▁events , ▁thereby ▁ident ifying ▁the ▁single ▁components ▁of ▁the ▁predicted ▁SS M ▁neut r ino ▁emission . ▁Finally , ▁ ▁K ami ok ande , ▁Super - K ami ok ande , ▁S NO , ▁B ore x ino ▁and ▁Kam L AND ▁used ▁el astic ▁scatter ing ▁on ▁electrons , ▁which ▁allows ▁the ▁measurement ▁of ▁the ▁neut r ino ▁energy . ▁Bor on 8 ▁neut r inos ▁have ▁been ▁seen ▁by ▁K ami ok ande , ▁Super - K ami ok ande , ▁S NO , ▁B ore x ino , ▁Kam L AND . ▁B ery l li um 7 , ▁p ep , ▁and ▁P P ▁neut r inos ▁have ▁been ▁seen ▁only ▁by ▁B ore x ino ▁to ▁date . ▁ ▁he p ▁neut r inos ▁The ▁highest ▁energy ▁neut r inos ▁have ▁not ▁yet ▁been ▁observed ▁due ▁to ▁their ▁small ▁flux ▁compared ▁to ▁the ▁bor on - 8 ▁neut r inos , ▁so ▁thus ▁far ▁only ▁limits ▁have ▁been ▁placed ▁on ▁the ▁flux . ▁No ▁experiment ▁yet ▁has ▁had ▁enough ▁sens itivity ▁to ▁observe ▁the ▁flux ▁predicted ▁by ▁the ▁SS M . ▁ ▁C NO ▁cycle ▁Ne ut r inos ▁from ▁the ▁C NO ▁cycle ▁of ▁solar ▁energy ▁generation ▁– ▁i . e ., ▁the ▁C NO - neut r inos ▁– ▁ ▁are ▁also ▁expected ▁to ▁provide ▁observable ▁events