A Note on the Mass of 27 Canis Majoris

It is shown that in range of velocity, length of period, correlation of emission and velocity changes, and in the presence of a secondary oscillation of short-period and smaller range than the main period, 27 Canis Majoris is a normal Be spectrum variable. Large variations in the periods of stars of this type rule out the hypothesis of orbital motion, and with it the enormous mass function derived by Struve. The supposed secondary spectrum is also a normal phenomenon of Be variables, and is due to a wing of the broad absorption which underlies and borders the emission lines