Analysis of the First Rocket Ultraviolet Solar Spectra.

Solar spectra obtained from V-2 ffights on October 10, 1946, and March 7, 1947, were analyzed. The spectrum in the hitherto unobserved region from 2900 to 2200 A was found to be intensely complex and filled with unresolved blends. The low resolution (1.5 A) made positive identification difficult ii~ many instances. Tables showing the wave length, visual estimated intensities, character, and identification of the lines observed are given. Reproductions of densitometer traces are given, and part of the spectrum is shown replotted on an intensity scale. Certain multiplets of Fe i, Fe ii, Si i, and Mnii appeared in great strength. Four lines-Si i, 2882 A; Mgi, 2852 A; Mg ii, 2803 A; and Mg ix, 2796 A-were very broad, similar to H and K of Can. The Mg ii pair showed a central core of emission of great strength. The structure between 2200 and 2300 A could not be interpreted in terms of atomic lines and may be caused by atmospheric bands of NO