The spectroscopic observations taken during the international Lyrae campaign of 1959 are discussed. These show no evidence for the effect of a third body on the velocity of the primary star or changes in the shape of its orbit. Accompanying the differences in light of up to 005 mag. between two successive eclipses are differences in the strengths and velocities of the helium lines formed in the expanding shell around the primary star. In general, the shell lines are stronger during cycles when the shell absorbs more continuous light near primary minimum, although instantaneously this correlation does not seem to be valid.