Iron abundance in the solar photosphere. Application of a two-component model atmosphere

Details Iron abundance in the solar photosphere. Application of a two-component model atmosphere Iron abundance in the solar photosphere. Application of a two-component model atmosphere

Aug 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002a%26a...391..331b&link_type=abstract

Astronomy and Astrophysics, v.391, p.331-337 (2002)

Astronomy and Astrophysics

Astrophysics

10

Sun: Photosphere, Line: Profiles, Sun: Abundances, Stars: Atmospheres, Stars: Abundances

Scientific paper

A realistic two-component model of the quiet Sun is used to determine the solar abundance of iron from the inversion of a number of Fe I and Fe II spectral lines for which accurate atomic parameters (oscillator strengths, central wavelengths, and collisional broadening cross sections) exist. From 33 Fe I lines we infer an abundance of A_Fe = 7.43 +/- 0.06, whereas we estimate A_Fe = 7.45 +/- 0.08 from 10 Fe II lines. These values are in excellent agreement with the results of analyses based on realistic 3D hydrodynamical simulations of the solar granulation, and imply a low photospheric iron abundance. We investigate the effects of convective motions and granular temperatures and conclude that both are important for reliable abundance determinations. For Fe I lines, the effects of convective motions can be simulated by using a microturbulent velocity of about 1 km s-1, whereas it is possible to account for temperature inhomogeneities by adopting an average temperature stratification which is cooler than the Holweger & Müller model in the upper layers.

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