Abstract
During solar flares, the Bragg Crystal Spectrometer (BCS) on Yohkoh observes the resonance (1s 2 1 S 0 – 1s2p 1 P 1, symbolised w) lines of He-like S, Ca, and Fe ions and neighbouring spectral regions, and exceptionally, during large flares, the Ly-α lines of H-like Fe. The contribution functions G(T e ), describing the emissivity as a function of electron temperature T e , peak at about 14, 35, and 70 MK (1 MK = 106 K). The G(T e ) curves cover a very broad range of temperature and overlap each other considerably. Spectra from the Yohkoh BCS and other spacecraft instruments that have been flown in recent years have been analyzed to give temperatures T e from the ratio of nearby dielectronic satellite lines to the resonance line. The theory is described by Gabriel (1972). Standard software packages (Morrison 1994) are available for doing this analysis.KeywordsEmission MeasureContribution FunctionLarge FlareStandard Software PackageFraction feTeThese keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.
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