Abstract
In order to resolve clusters of X-ray lines emitted by flares (Fritz et al , 1967; Neupert and Swartz, 1970) and to determine line shapes, a considerable resolving power is needed. The angular size of flares, typically about 2’ will not allow the necessary resolution to be obtained without a very fine slit system combined with the flat crystal X-ray spectrometer. In stellar X-ray spectroscopy large plane diffracting crystals will be associated with large counters, which in turn would act as a source of considerable noise.
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