The source region of the slow solar wind is complicated by the fact that it is apparently located at the boundary between the helmet streamer belt arcade and adjacent polar coronal holes. This location implies that it should occupy the same region of heliospheric space as transients associated with CMEs, and may in fact consist partly of slow transients. Here we suggest a way to visualize the transient source using sequential potential field source surface models of the coronal magnetic field. We also suggest how future analysis of heat flux electron anisotropies could be used to empirically determine the transient contribution to the slow solar wind.