Compton Backscattering of Solar X-Ray Emission
Abstract
Compton backscattering of solar flare emission, X < 2 A, appears to have several interesting effects when X-ray spectra are considered in detaiL Line emission generates secondary spectra shifted up to 0.08 A, thereby broadening the long-wavelength wing. The iron lines at 1.9 A are discussed in detail, and the observed spectra obtained between 1.88 and 1.92 A are shown to be significantly affected by Compton backscattering for flares occurring on the solar disk. The rapid decrease in the photoelectric crosssection causes the Compton backscattering contribution to increase from S to 50 percent over the region from 2.5 to 0.3 A. This implies substantial corrections to emission measures obtained from high-energy solar events. Flare temperatures inferred from the corrected continuum shape may be reduced as much as 20 percent. The iron abundance in the photosphere deduced from the iron Ka fluorescence line at 1.932 A does not appear to be sufficient to generate an observable change in the Compton reflectivity at the iron K-shell edge at 1.74 A.
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