On the determination of the solar iron abundance using Fe I lines.

Details On the determination of the solar iron abundance using Fe I lines. On the determination of the solar iron abundance using Fe I lines.

Apr 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...296..217b&link_type=abstract

Astronomy and Astrophysics, v.296, p.217

Astronomy and Astrophysics

Astrophysics

102

Sun: Abundances, Atomic Data

Scientific paper

There presently exist two main-stream solar iron abundances determined using Fe I lines; a `high' value of which 7.67+/-0.03 (Blackwell et al. 1984) is typical, and a `low' value typified by 7.50+/-0.07 (Holweger et al. 1991). The `low' abundance agrees with determinations using Fe II lines, and with the meteoritic value. The two Fe I values differ by 48 per cent. An in-depth discussion of the two results, and possible reasons for their difference, is given in the present paper. It is concluded that the Fe I lines with excitation energy less than 2.6eV do indeed show a `high' abundance when interpreted using the Holweger-Mueller empirical model atmosphere. The adoption of less accurate oscillator strengths and equivalent widths, and less suitable damping constants, all account, in our opinion, for the `low' value found by Holweger et al. (1991). However, analyses identical to those of Blackwell et al. (1984) which use the Kurucz (ATLAS9) and the new MARCS model atmospheres instead of the Holweger-Mueller empirical atmosphere, show a `low' abundance in reasonable agreement with the results of Fe II analyses and the meteoritic determination. These numerical models, however, are less successful at reproducing observed limb-darkening than the Holweger-Mueller empirical model, although the ATLAS9 model reproduces the ultraviolet continuous flux better than the Holweger-Mueller atmosphere. Existing numerical and empirical solar model atmospheres would therefore appear to be inadequate; they cannot both match the observed limb-darkening and emergent flux, and give a consistent iron abundance determination based on Fe I and Fe II lines of all excitations.

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