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198 4MNRAS.210..443V 444 N. J. Veck et al. observations are best fitted qualitatively by a model where pre-existing magnetic loop structures are perturbed by the intrusion of new magnetic flux. After the main phase of the flare, the height of the Ha loops and the region of X-ray emission gradually increase, perhaps involving further loop systems. Comparisons with flare models are made.

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A comparison is made between Ca xlx and Ca xvIIl line ratios observed in solar flares with the Bent Crystal Spectrometer (BCS) on the Solar Maximum Mission (SMM) satellite and currently available atomic data. Close agreement is found with the excitation rates recently published by Pradhan et al. (1981). The observations show little dependence of line ratios on electron temperature, supporting a further conclusion that cascade contributions to the 23p and 23S levels are not significant,

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