Spectral and photometric observations of the star Y Ori

Data are presented from a spectral and photometric study of the long-period variable star Y Ori, which we have classified as a type M7IIIe near its brightness minimum. In the blue part of the spectrum, features from a star of an earlier spectral class are superimposed on the spectrum of a cool giant, so that a variable excess emission is observed at wavelengths of 4000–4200 Å. As opposed to the monotonically decreasing intensity of the Balmer lines ( EWH α > EWH β > EWH γ > EWH δ) in normal stars belonging to the earlier spectral classes, a reverse relationship, with EWH γ < EWH δ is detected in Y Ori.