▁four ▁pro tons ▁are ▁combined ▁to ▁produce ▁two ▁pro tons , ▁two ▁neut rons , ▁two ▁posit rons , ▁and ▁two ▁electron ▁neut r inos . ▁ ▁Ne ut r inos ▁are ▁also ▁produced ▁by ▁the ▁C NO ▁cycle , ▁but ▁that ▁process ▁is ▁consider ably ▁less ▁important ▁in ▁the ▁Sun ▁than ▁in ▁other ▁stars . ▁ ▁Most ▁of ▁the ▁neut r inos ▁produced ▁in ▁the ▁Sun ▁come ▁from ▁the ▁first ▁step ▁of ▁the ▁pp ▁chain ▁but ▁their ▁energy ▁is ▁so ▁low ▁( < 0 . 4 2 5 ▁Me V ) ▁they ▁are ▁very ▁difficult ▁to ▁detect . ▁ ▁A ▁rare ▁side ▁branch ▁of ▁the ▁pp ▁chain ▁produces ▁the ▁" bor on - 8 " ▁neut r inos ▁with ▁a ▁maximum ▁energy ▁of ▁roughly ▁ 1 5 ▁Me V , ▁and ▁these ▁are ▁the ▁easiest ▁neut r inos ▁to ▁detect . ▁ ▁A ▁very ▁rare ▁interaction ▁in ▁the ▁pp ▁chain ▁produces ▁the ▁" he p " ▁neut r inos , ▁the ▁highest ▁energy ▁neut r inos ▁predicted ▁to ▁be ▁produced ▁by ▁the ▁Sun . ▁ ▁They ▁are ▁predicted ▁to ▁have ▁a ▁maximum ▁energy ▁of ▁about ▁ 1 8 ▁Me V . ▁ ▁All ▁of ▁the ▁interactions ▁described ▁above ▁produce ▁neut r inos ▁with ▁a ▁spectrum ▁of ▁energ ies . ▁ ▁The ▁electron ▁capture ▁of ▁ 7 Be ▁produces ▁neut r inos ▁at ▁either ▁roughly ▁ 0 . 8 6 2 ▁Me V ▁( ~ 9 0 %) ▁or ▁ 0 . 3 8 4 ▁Me V ▁( ~ 1 0 %). ▁