▁This ▁theory ▁allows ▁predictions ▁to ▁be ▁made ▁about ▁how ▁particles ▁will ▁interact ▁under ▁many ▁conditions . ▁The ▁energy ▁per ▁particle ▁in ▁a ▁super n ova ▁is ▁typically ▁ 1 – 1 5 0 ▁p ico jou les ▁( t ens ▁to ▁hundreds ▁of ▁Me V ). ▁The ▁per - part icle ▁energy ▁involved ▁in ▁a ▁super n ova ▁is ▁small ▁enough ▁that ▁the ▁predictions ▁gained ▁from ▁the ▁Standard ▁Model ▁of ▁particle ▁physics ▁are ▁likely ▁to ▁be ▁basically ▁correct . ▁But ▁the ▁high ▁dens ities ▁may ▁require ▁corre ctions ▁to ▁the ▁Standard ▁Model . ▁In ▁particular , ▁Earth - based ▁particle ▁acceler ators ▁can ▁produce ▁particle ▁interactions ▁which ▁are ▁of ▁much ▁higher ▁energy ▁than ▁are ▁found ▁in ▁super nov ae , ▁but ▁these ▁experiments ▁involve ▁individual ▁particles ▁interact ing ▁with ▁individual ▁particles , ▁and ▁it ▁is ▁likely ▁that ▁the ▁high ▁dens ities ▁within ▁the ▁super n ova ▁will ▁produce ▁novel ▁effects . ▁The ▁interactions ▁between ▁neut r inos ▁and ▁the ▁other ▁particles ▁in ▁the ▁super n ova ▁take ▁place ▁with ▁the ▁weak ▁nuclear ▁force , ▁which ▁is ▁believed ▁to ▁be ▁well ▁understood . ▁However , ▁the ▁interactions ▁between ▁the ▁pro tons ▁and ▁neut rons ▁involve ▁the ▁strong ▁nuclear ▁force , ▁which ▁is ▁much ▁less ▁well ▁understood . ▁ ▁The ▁major ▁un sol ved ▁problem ▁with ▁Type   II ▁super nov ae ▁is ▁that ▁it ▁is ▁not ▁understood ▁how ▁the ▁burst ▁of ▁neut r inos ▁trans fers ▁its ▁energy ▁to ▁the ▁rest ▁of ▁the ▁star ▁producing ▁the ▁shock ▁wave ▁which ▁causes ▁the ▁star ▁to ▁expl