The Analysis of XUV Emission Lines
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.
- Publication:
-
Solar Physics
- Pub Date:
- December 1975
- DOI:
- 10.1007/BF00158452
- Bibcode:
- 1975SoPh...45..301W
- Keywords:
-
- Far Ultraviolet Radiation;
- Solar Corona;
- Solar Spectra;
- Solar Temperature;
- Ultraviolet Spectra;
- Abundance;
- Line Spectra;
- Oso;
- Solar Physics;
- Spectral Line;
- Intensity Measurement;
- Emission Line;
- Line Intensity;
- Heavy Element