The Maia Stars - a Real Class of Variable Stars

In 1955, O. Struve suggested that a sequence of variable stars having periods between about 0.1-0.3d and spectral types in the range B7III-A2 V-II might exist. These stars were called "Maia" stars after the presumed prototype Pleiadid, Maia. Struve later abandoned this proposal when he concluded that Maia was neither a light nor velocity variable. Despite Struve's disclaimer, the search for short period variability in this spectral region has continued. This paper summarizes the observational data relating to the "Maia" variables and suggests that little if any reason exists for maintaining the "Maia star" designation.