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Astron. Astrophys. 347, 348-354 (1999)


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The solar abundance of iron and the photospheric model *

N. Grevesse 1 and A.J. Sauval 2

1 Institut d'Astrophysique et de Géophysique, Université de Liège, avenue de Cointe, 5, B-4000 Liège, Belgium (grevesse@astro.ulg.ac.be)
2 Observatoire Royal de Belgique, avenue circulaire, 3, B-1180 Bruxelles, Belgium (Jacques.Sauval@oma.be)

Received 22 March 1999 / Accepted 23 April 1999

Abstract

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, [FORMULA] = 7.50 [FORMULA] 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 (130.79.128.5) (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

© European Southern Observatory (ESO) 1999

Online publication: June 18, 1999

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