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A prominent emission feature frequently observed in the solar X-ray spectrum near 1.9 A at times of chromospheric flares is found, from data obtained by the Fifth Orbiting Solar Observatory, to consist of at least six spectral lines. In addition to the , , and possibly the 1'S0-23S1 transitions of Fe xxv, there appear to be satellite lines originating in highly excited Fe xxiv, Fe XXIII, and lower stages of ionization.
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Neupert et al. (1970) studied this question.
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