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The present state of knowledge of the spectrum of the sun from 3000 ~ to 170 A. is critically reviewed. The characteristics of the different photographic and photoelectric spectroscopic instruments and the results are summarized and compared. Topics covered are line identifications, intensities, the continuum and its origin, the sun's surface in Lyman alpha, the profiles of H and K of Mg II, Lyman alpha and beta, and monitoring work conducted from rockets and satellites, including OSO-I.

Forbidden lines of Fe xvm, Fe xix, and Fe xxi are identified at 974, 1118, and 1354 Ä, respectively, in NRL ATM solar flare spectra. These lines are due to magnetic dipole transitions between levels of the ground configurations. The widths of the Fe xix and Fe xxi lines are ^0.5 Ä, which is substantially greater than expected in ionization equilibrium. The intensity-time behavior and the widths of these lines are discussed for the 1973 June 15 flare.