satisfy this criteria, although the outer shells for MS14 and MS4 do not. Therefore, 12 of the 48 WR stars we observe (25$\%$) may be surrounded by “classical” WR E- or W-type shells. The remaining 11 Group Ia shells contain three or more stars, or have a radii $>$40 pc, and are probably R-type.

Previous observations have suggested Galactic E- and W-type shells are generally $<$20 pc in radius (Chu 1981; Marston 1997). Our data (in particular see Figure 4), on the other hand, suggest that the shells of this type [*may*]{} be larger in M31, on average, than their Galactic counterparts. However, some of our larger shells (including those classified as R-type) may be (and in some instances probably are) classical, ring-like regions or, for the very largest shells, “superbubbles” (e.g. Oey & Massey 1994; Oey 1996), and may not be “classical” WR ring nebulae. Future observations to specifically classify the shells presented in this paper, as either E-, W- or R-type, would be necessary to verify that E- or W-shells are indeed larger in M31 than the Galaxy.

WR ring nebulae in the Galaxy and LMC have revealed interesting statistical trends, suggesting WC stars generally are found within 