THE unusual brightness of the corona at the 1936 total eclipse—it was easily seen several seconds before totality began—has given Prof. Sekiguti and his colleagues the chance of obtaining some new lines in the emission spectrum of the corona. Confirming Prof. Tanaka, he restores the line at 4725 A., previously rejected as being insufficiently supported, to the list, and points out that this line and several other lines are close to, if not identical with, certain lines in the spectra of nebulae and novae. His new spectral lines strengthen the link between the coronal and nova spectra based previously solely on the presence of the stronger coronal lines in the spectrum of RS Ophiuchi a few weeks after its outburst in 1933.