If Population II main‐sequence stars have winds similar to the solar wind, then these stars could provide a feasible mechanism for expelling red‐giant ejecta from globular clusters. For clusters having line‐of‐sight velocity dispersions less than 22 km s −1 , the mass and energy output of main‐sequence star winds is found to be sufficient to establish a cluster outflow which is capable of removing all red‐giant ejecta. This mechanism provides a natural means for continuously sweeping all or most globular clusters of stellar ejecta.
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Graeme H. Smith (1999) studied this question.
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