▁ten - second ▁burst . ▁Also , ▁the ▁collapse ▁of ▁the ▁inner ▁core ▁is ▁halt ed ▁by ▁neut ron ▁deg ener acy , ▁causing ▁the ▁impl os ion ▁to ▁re bound ▁and ▁b ounce ▁out ward . ▁The ▁energy ▁of ▁this ▁expand ing ▁shock ▁wave ▁is ▁sufficient ▁to ▁dis rupt ▁the ▁over lying ▁stell ar ▁material ▁and ▁acceler ate ▁it ▁to ▁escape ▁velocity , ▁forming ▁a ▁super n ova ▁explos ion . ▁The ▁shock ▁wave ▁and ▁extremely ▁high ▁temperature ▁and ▁pressure ▁rapidly ▁diss ip ate ▁but ▁are ▁present ▁for ▁long ▁enough ▁to ▁allow ▁for ▁a ▁brief ▁period ▁during ▁which ▁the ▁production ▁of ▁elements ▁heav ier ▁than ▁iron ▁occurs . ▁Depending ▁on ▁initial ▁mass ▁of ▁the ▁star , ▁the ▁rem n ants ▁of ▁the ▁core ▁form ▁a ▁neut ron ▁star ▁or ▁a ▁black ▁hole . ▁Because ▁of ▁the ▁underlying ▁mechanism , ▁the ▁resulting ▁super n ova ▁is ▁also ▁described ▁as ▁a ▁core - collapse ▁super n ova . ▁ ▁There ▁exist ▁several ▁categories ▁of ▁Type   II ▁super n ova ▁explos ions , ▁which ▁are ▁categor ized ▁based ▁on ▁the ▁resulting ▁light ▁curve — a ▁graph ▁of ▁lum inos ity ▁versus ▁time — follow ing ▁the ▁explos ion . ▁Type   II - L ▁super nov ae ▁show ▁a ▁steady ▁( linear ) ▁decl ine ▁of ▁the ▁light ▁curve ▁following ▁the ▁explos ion , ▁whereas ▁Type   II - P ▁display ▁a ▁period ▁of ▁slower ▁decl ine ▁( a ▁plate au ) ▁in ▁their ▁light ▁curve ▁followed ▁by ▁a ▁normal ▁decay . ▁Type  