shells based solely on imaging data, we attempt to determine which shells may be physically associated with WR stars based on criteria discussed below. Excess point source H$\alpha$ emission associated with WR stars might indicate unresolved E- or W-shells, or emission from a WR stellar wind. The Galactic WNL star HDE 313846 has a broad H$\alpha$ emission line, with an equivalent width of 23 ${\rm \AA}$, which has been interpreted as arising in an extended outer envelope indicating a strong stellar wind (Crowther & Bohannan 1997). For this reason we also list the stars with unresolved H$\alpha$ excess.

The paper is organized as follows. In $\S$2 and 3 we present details of the observations and data reduction. In $\S$4 we describe our morphological classification of H$\alpha$ emission near WR stars, present H$\alpha$ and B images, and provide the physical properties of all detected shells. Further, we attempt to determine which shells are causally associated with a WR star. We discuss the environments of WR stars, and evidence for WR wind-ISM interactions, in $\S$5. We present our summary and conclusions in $\S$6.

THE OBSERVATIONS
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The data relevant to this study include previously published and new imaging data of M31, both 