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The solar abundance of iron and the photospheric model *
N. Grevesse 1 and
A.J. Sauval 2
Received 22 March 1999 / Accepted 23 April 1999
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, = 7.50 0.05, which perfectly agrees with the meteoritic value.
Key words: atomic data Sun: abundances Sun: photosphere
* A detailed version of Table 2 is available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (18.104.22.168) (ftp://cdsarc.u-strasbg.fr/pub/cats/J/A+A/347/348 ) or at the ORB via anonymous ftp to ftp://ftpserver.oma.be/pub/astro/jacques.
Send offprint requests to: A.J. Sauval
Online publication: June 18, 1999