Of the steadily increasing number of Doppler Images appearing in the literature, the majority are of the RS CVn subclass of binary stars. The large rotational velocities and dynamo action of these stars is probably attributable to tidal spin-up of the active subgiant star by its binary companion. Their dynamos and resultant surface features (starspots) are thus almost certainly influenced by the companion. As such, these objects are not the ideal testing ground for comparison with single-star solar-like activity. Recently, a handful of Doppler images of single late-type main sequence and pre-main sequence stars have appeared in the literature. Pre-main sequence stars include V410 Tau (Joncour, Bertout, & Menard 1994), (Strassmeier, Welty, & Rice 1994), (Hatzes 1995) and HD 283572 (Joncour, Bertout, & Bouvier 1994). The main sequence stars include AB Dor (Collier Cameron & Unruh 1994), (Kürster, Schmitt, & Cutispoto 1994) and LQ Hya (Strassmeier, et al. 1993), (Saar & Piskunov 1994). These studies suggest that high-latitude dark spots are common to all rapidly-rotating stars, although, the spots found in the above work do not symmetrically straddle the pole as do polar spots of rapidly-rotating RS CVn binary stars.