PRIMEVAL WINDS WITHIN GLOBULAR-CLUSTERS

Early stellar mass-loss rates within Galactic globular clusters were l ikely to have been much larger than at present. Within the most tightl y bound globular clusters a substantial intracluster medium could have been acquired during the epoch when the main-sequence turn-off mass w as around 5 M.. By contrast, the stellar ejecta are likely to have bee n lost entirely from clusters having small binding energies, either st ochastically through the expansion of discrete mass-loss shells, or vi a outflow within a continuous intracluster wind. Criteria for the esta blishment of continuous winds within globular clusters are obtained fr om a consideration of the cluster escape velocities and the expected r ate of stellar mass-ejection events. If mass loss from intermediate-ma ss stars was characterized by ejection speeds of approximate to 20 km s(-1), it is concluded that a number of Galactic globular clusters may have been the sites of primeval winds. It is found that the accretion of material from such a wind, even if it were pure nitrogen, would be insufficient to account for the nitrogen enhancements observed among some CN-strong cluster giants. In particular, the CN enhancements obse rved among some stars in low-mass clusters such as Palomar 5 are unlik ely to have been produced by accretion, unless such clusters were init ially much more massive than at present.