Astronomy and Astrophysics – Astronomy
Scientific paper
May 1977
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977a%26a....57..185p&link_type=abstract
Astronomy and Astrophysics, vol. 57, no. 1-2, May 1977, p. 185-191.
Astronomy and Astrophysics
Astronomy
31
Abundance, Solar Corona, Solar X-Rays, X Ray Astronomy, Iron, Magnesium, Neon, Nickel, Oxygen Atoms, Photosphere, Silicon, Sodium, Solar Cosmic Rays, Ultraviolet Spectroscopy, X Ray Spectra
Scientific paper
A method for determining relative coronal abundances on the basis of solar X-ray observations is discussed which employs resonance lines of one- and two-electron ions and does not require a model of the emitting region. The method is used to determine O:Ne, Ne:Mg, Mg:Fe, Mg:Na, Fe:Ni, and Mg:Si relative abundance ratios that depend only on the oscillator strengths of the ions involved, their emission functions, and the observed flux ratios. The results are compared with previous determinations based on X-ray, UV, photospheric, and solar-cosmic-ray observations as well as meteoritic analyses. Logarithmic abundances relative to Si are calculated and found to be consistent with other measurements except for O. The origin of the discrepancy is briefly considered.
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