▁many ▁small ▁fl ares ▁contrib uting ▁to ▁the ▁" qu ies cent " ▁X - ray ▁emission ▁from ▁these ▁stars . ▁Pre – main ▁sequence ▁stars ▁have ▁large ▁con ve ction ▁zones , ▁which ▁in ▁turn ▁drive ▁strong ▁dynam os , ▁producing ▁strong ▁surface ▁magnetic ▁fields . ▁This ▁leads ▁to ▁the ▁high ▁X - ray ▁emission ▁from ▁these ▁stars , ▁which ▁lie ▁in ▁the ▁s atur ated ▁X - ray ▁regime , ▁unlike ▁main - sequence ▁stars ▁that ▁show ▁rot ational ▁mod ulation ▁of ▁X - ray ▁emission . ▁Other ▁sources ▁of ▁X - ray ▁emission ▁include ▁acc ret ion ▁hot sp ots ▁and ▁col lim ated ▁out flow s . ▁ ▁X - ray ▁emission ▁as ▁an ▁indicator ▁of ▁stell ar ▁youth ▁is ▁important ▁for ▁studies ▁of ▁star - form ing ▁regions . ▁Most ▁star - form ing ▁regions ▁in ▁the ▁Mil ky ▁Way ▁Gal axy ▁are ▁project ed ▁on ▁Gal actic - Pl ane ▁fields ▁with ▁numerous ▁un related ▁field ▁stars . ▁It ▁is ▁often ▁impossible ▁to ▁distinguish ▁members ▁of ▁a ▁young ▁stell ar ▁cluster ▁from ▁field - star ▁cont amin ants ▁using ▁optical ▁and ▁inf ra red ▁images ▁alone . ▁X - ray ▁emission ▁can ▁easily ▁pen et rate ▁moder ate ▁absor ption ▁from ▁mole cular ▁clouds , ▁and ▁can ▁be ▁used ▁to ▁identify ▁candidate ▁cluster ▁members . ▁ ▁Un stable ▁wind s ▁Given ▁the ▁lack ▁of ▁a ▁significant ▁outer ▁con ve ction ▁zone , ▁theory ▁predict s ▁the ▁absence ▁of ▁a ▁magnetic ▁dynam o ▁in ▁earlier ▁A ▁stars .