Evidence for the equality of the solar photospheric and coronal abundance of iron
Abstract
The Fe Kalpha and Kbeta X-ray lines (wavelengths 1.94 and 1.76 Angstroms) in the solar X-ray spectrum are formed by fluorescence of photospheric iron atoms, and the ratio of the intensity of either to the He-like iron (Fe xxv) resonance line at 1.85 Angstroms is a function of the photospheric-to-coronal abundance of iron. The temperature dependence of this ratio is weak as long as the flare temperature T_e>^⋈ 15 x 10^6K. Comparison of the theoretical value of this intensity ratio with observations from crystal spectrometers on Yohkoh, SMM and P78-1 are consistent with the photospheric abundance of Fe being equal to the coronal.
- Publication:
-
Advances in Space Research
- Pub Date:
- July 1995
- Bibcode:
- 1995AdSpR..15g..33P
- Keywords:
-
- Abundance;
- Iron;
- K Lines;
- Photosphere;
- Solar Corona;
- Solar X-Rays;
- Stellar Models;
- X Ray Astronomy;
- X Ray Spectra;
- Hydrogen;
- Solar Flares;
- Solar Maximum Mission;
- Solar Spectrometers;
- Solar Temperature;
- X Ray Fluorescence;
- Solar Physics