The analysis of XUV emission lines

A technique for analyzing measurements of XUV spectral line intensities is described. Application of the technique to OSO-4 and OSO-6 spectra indicates that the mean coronal temperature is 2.1X106K in typical active solar regions and that the mean coronal temperature in typical quiet regions ranges from 1.5X106 to 2.1X106K. One active region spectrum shows evidence for substantial quantities of coronal material with 2X106<T<3.5X106K. Measurements from limb spectra show evidence that (1) coronal abundances of N and O are low relative to heavier elements; or (2) that the ionization equilibrium calculations used may contain systematic errors; or (3) that the XUV intensity measurements may be incorrectly calibrated. (Auth.)