The abundance of iron in the sun derived from photospheric Fe II lines

Details The abundance of iron in the sun derived from photospheric Fe II lines The abundance of iron in the sun derived from photospheric Fe II lines

Jun 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...232..510h&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 232, no. 2, June 1990, p. 510-515.

Astronomy and Astrophysics

Astrophysics

137

Abundance, Iron, Line Spectra, Photosphere, Solar Granulation, Solar Spectra, Atmospheric Models, Hollow Cathodes, Meteoritic Composition, Silicon

Scientific paper

The solar abundance of iron is determined from photospheric Fe II lines whose f-values have been measured recently in a hollow-cathode experiment. In contrast to lines of Fe I these lines are perfectly in LTE in the sun, and the derived abundance is insensitive to imperfect modeling of the solar photosphere. The resulting iron abundance, log N (Fe) = 7.48 + or - 0.09 on the scale log N (H) = 12, is significantly lower than the currently accepted value based on lines of Fe I. The solar Fe/Si abundance ratio agrees with the meteoritic value found in C1 chrondrites. The resulting solar Fe I/Fe II abundance discrepancy is discussed.

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