Spectrum of γ Cassiopeiæ

Abstract

SINCE photography was first applied for recording the spectrum of this bright star, its spectrum has always been considered to be of a constant character. In 1928, I announced that a slight change had taken place, and since then I have made numerous observations which completely corroborate its variability. The relative intensities of the bright components of the hydrogen lines in the latter half of 1931 were such that the red components were a little brighter than the violet components. Since then, the violet components have been steadily increasing in intensity, and now (January) they are very much stronger than the red components, so much so that, in the case of Hε and Hζ, the red components are scarcely visible while the violet components are quite strong.