Differences in the fractions of Be stars in galaxies

The number ratios Be/(B + Be) of Be to B-type stars in young, well studied clusters of the Galaxy, the LMC and SMC are examined. In order to disentang le age and metallicity effects we choose clusters in the same age interval and for which reliable photometric and spectroscopic data are available. Nu mber counts are made for various magnitude intervals, and the results are f ound to be stable with respect to this choice. In the magnitude interval M- V = -5 to -1.4 (i.e. O9 to B3) we obtained a ratio Be/(B + Be) = 0.11, 0.19 , 0.23, 0.39 for 21 clusters located in the interior of the Galaxy, the ext erior of the Galaxy, the LMC and the SMC, respectively. Various hypotheses for these differences are examined. An interesting possi bility is that the average rotation is faster at low metallicities as a res ult of star formation processes. The much higher relative N-enrichment foun d by Venn et al. (1998) in A-type supergiants of the SMC, compared to galac tic supergiants, also strongly supports the presence of more rotational mix ing at low metallicities. We discuss whether high rotational mixing may be the source of primary nitrogen in the early chemical evolution of galaxies.