Abstract
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 2.1 × 106 K in typical active solar regions and that the mean coronal temperature in typical quiet regions ranges from 1.5 × 106 to 2.1 × 106 K. One active region spectrum shows evidence for substantial quantities of coronal material with 2 × 106 < T < 3.5 × 106 K. 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.
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a call
