1996PASP..108..176S

Early stellar mass-loss rates within Galactic globular clusters were likely to have been much larger than at present. Within the most tightly bound globular clusters a substantial intracluster medium could have been acquired during the epoch when the main sequence turn-off mass was around 5 solar mass. By contrast, the stellar ejecta are likely to have been lost entirely from clusters having small binding energies, either stochastically through the expansion of discrete mass-loss shells, or via outflow within a continuous intracluster wind. Criteria for the establishment of continuous winds within globular clusters are obtained from a consideration of the cluster escape velocities and the expected rate of stellar mass ejection events. If mass loss from intermediate-mass stars was characterized by ejection speeds of ∼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 observed among some stars in low-mass clusters such as Palomar 5 are unlikely to have been produced by accretion, unless such clusters were initially much more massive than at present.