We present spectrophotometry of the strongest emission-line features for the eight known Wolf-Rayet (W-R) stars in the Small Magellanic Cloud (SMC). Seven are relatively "early" WN types; one is a WO. These are compared to stars of similar spectral types in the Galaxy and the Large Magellanic Cloud (LMC). Five or six of the W-R stars are binaries but in only four of these is the contribution of the companion to the continuum significant. In the other four WN type stars, the 4686 He II emission lines can be directly compared to single stars of similar type; in these objects the lines are weak, suggesting the stellar winds are not as strong as comparable stars in the Galaxy and LMC. The other emission lines, particularly those due to various nitrogen ions, are also weak, but no more so than would have been expected given the weakness in the helium features. Thus the hydrogen-burning CNO cycle "equilibrium" nitrogen abundance with respect to helium appears to be similar to that in WN stars of the Galaxy and LMC even though the SMC objects presumably began their lives with appreciably smaller CNO content.
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Conti et al. (1989) studied this question.