The solar abundance of iron and the photospheric model

Details The solar abundance of iron and the photospheric model The solar abundance of iron and the photospheric model

Jul 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999a%26a...347..348g&link_type=abstract

Astronomy and Astrophysics, v.347, p.348-354 (1999)

Astronomy and Astrophysics

Astrophysics

149

Atomic Data, Sun: Abundances, Sun: Photosphere

Scientific paper

Numerous papers on the solar photospheric abundance of iron have recently been published leading to a longstanding debate concerning rather different results obtained from the analyses of Fe i lines and, to a lesser extent, of Fe ii lines. Based on a set of 65 solar Fe i lines, with accurate transition probabilities as well as new accurate damping constants, we construct a new empirical photospheric model. We succeed to reconcile abundance results obtained from low and high excitation Fe i lines as well as from Fe ii lines and derive a solar photospheric abundance of iron, A_Fe = 7.50 +/- 0.05, which perfectly agrees with the meteoritic value. A detailed version of Table~2 is available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or at the ORB via anonymous ftp to ftpserver.oma.be/pub/astro/jacques.

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