▁distribution ▁as ▁functions ▁of ▁distance ▁to ▁the ▁nucle us ▁and ▁the ▁com et ary - sol ar ▁wind ▁interaction . ▁ ▁During ▁the ▁encounter , ▁V ega ▁ 2 ▁took ▁ 7 0 0 ▁images ▁of ▁the ▁com et , ▁with ▁better ▁resolution ▁than ▁those ▁from ▁the ▁tw in ▁V ega ▁ 1 , ▁partly ▁due ▁to ▁the ▁presence ▁of ▁less ▁dust ▁outside ▁the ▁com a ▁at ▁the ▁time . ▁Yet ▁V ega ▁ 2 ▁recorded ▁an ▁ 8 0 % ▁power ▁loss ▁during ▁the ▁encounter ▁as ▁compared ▁to ▁V ega ▁ 1 ' s ▁ 4 0 %. ▁ ▁After ▁further ▁imag ing ▁sessions ▁on ▁ 1 0 ▁and ▁ 1 1 ▁March ▁ 1 9 8 6 , ▁V ega ▁ 2 ▁finished ▁its ▁primary ▁mission . ▁ ▁Post ▁Hal ley ▁ ▁A ▁ 6 ▁million ▁kilometer ▁distant ▁fly by ▁of ▁ 2 1 0 1 ▁Ad on is ▁was ▁considered ▁but ▁it ▁turned ▁out ▁that ▁V ega ▁ 2 ▁didn ' t ▁have ▁enough ▁fuel ▁left ▁to ▁make ▁the ▁necessary ▁orb ital ▁changes ▁for ▁the ▁fly by . ▁Instead ▁the ▁V ega ▁prob es ▁took ▁the ▁opportunity ▁to ▁measure ▁the ▁dust ▁as ▁they ▁passed ▁through ▁the ▁or bits ▁of ▁ 7 2 P / Den ning – F uj ik awa , ▁B iel a ' s ▁Com et ▁and ▁ 2 8 9 P / B lan p ain . ▁ ▁Contact ▁with ▁V ega ▁ 2 ▁was ▁lost ▁on ▁ 2 4 ▁March ▁ 1 9 8 7