The 263.7-A line observed in solar flare spectra during the Skylab mission is identified as an intercombination line of Fe XXIII. The identification is confirmed by direct observation of the line along the isoelectronic sequence, including S XIII, Ar XV, Ca XVII, and Cr XXI. Observation of the beryllium sequence in solar flares is outlined, and the method of identification is described. Significant characteristics of the Fe XXIII and Fe XXIV images observed in the flare of June 15, 1973, are discussed and include an archlike spatial structure spanning the magnetic neutral line and a Doppler-widened emission core, which may pinpoint the site of the energy release.
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K. G. Widing (1975) studied this question.