▁young ▁stell ar ▁clusters ▁with ▁more ▁than ▁ 1 0 4 ▁stars ▁pc . − 3 ▁close ▁enc oun ters ▁between ▁stars ▁can ▁lead ▁to ▁interactions ▁between ▁pro top lan et ary ▁dis ks ▁that ▁affect ▁developing ▁planet ary ▁systems . ▁ ▁Young ▁stell ar ▁objects ▁ ▁Several ▁special ▁types ▁of ▁young ▁stell ar ▁object ▁have ▁been ▁identified ▁in ▁RC W ▁ 3 6 , ▁and ▁are ▁described ▁in ▁more ▁detail ▁below . ▁The ▁properties ▁of ▁these ▁stars ▁are ▁related ▁to ▁their ▁extreme ▁youth . ▁ ▁Two ▁stars ▁in ▁RC W ▁ 3 6 ▁have ▁Her big - H aro ▁j ets ▁( HH ▁ 1 0 4 2 ▁and ▁H H ▁ 1 0 4 3 ). ▁J ets ▁of ▁gas ▁flow ing ▁out ▁from ▁young ▁stars ▁can ▁be ▁produced ▁by ▁acc ret ion ▁onto ▁a ▁star . ▁In ▁RC W ▁ 3 6 ▁these ▁j ets ▁were ▁seen ▁in ▁a ▁number ▁of ▁spectral ▁lines , ▁including ▁lines ▁from ▁hydro gen , ▁hel ium , ▁o xygen , ▁nit ro gen , ▁sul fur , ▁nick el , ▁calci um , ▁and ▁iron . ▁Mass ▁loss ▁rates ▁from ▁the ▁j ets ▁have ▁been ▁estimated ▁to ▁be ▁on ▁the ▁order ▁of ▁ 1 0 − 7 ▁ ▁solar ▁masses ▁per ▁year . ▁In hom ogene ities ▁in ▁the ▁j ets ▁have ▁been ▁attributed ▁to ▁variable ▁acc ret ion ▁rate ▁on ▁times cal es ▁of ▁approximately ▁ 1 0 0 ▁years . ▁ ▁The ▁young ▁star ▁ 2 MA SS ▁J 0 8 5