Volume 573, January 2015
|Number of page(s)||33|
|Published online||11 December 2014|
The elemental composition of the Sun
II. The iron group elements Sc to Ni⋆
Department of Physics, Imperial College LondonBlackett
Laboratory, Prince Consort
SW7 2AZ, UK
2 Research School of Astronomy and Astrophysics, Australian National University, Cotter Rd., Weston Creek, ACT 2611, Australia
3 Centre Spatial de Liège, Université de Liège, avenue Pré Aily, 4031 Angleur-Liège, Belgium
4 Institut d’Astrophysique et de Géophysique, Université de Liège, Allée du 6 août, 17, B5C, 4000 Liège, Belgium
5 Institute of Astronomy, University of Cambridge, Madingley Road, CB3 0HA, Cambridge, UK
6 Observatoire Royal de Belgique, avenue circulaire, 3, 1180 Bruxelles, Belgium
Received: 1 May 2014
Accepted: 1 September 2014
We redetermine the abundances of all iron group nuclei in the Sun, based on neutral and singly-ionised lines of Sc, Ti, V, Mn, Fe, Co and Ni in the solar spectrum. We employ a realistic 3D hydrodynamic model solar atmosphere, corrections for departures from local thermodynamic equilibrium (NLTE), stringent line selection procedures and high quality observational data. We have scoured the literature for the best quality oscillator strengths, hyperfine constants and isotopic separations available for our chosen lines. We find log ϵSc = 3.16 ± 0.04, log ϵTi = 4.93 ± 0.04, log ϵV = 3.89 ± 0.08, log ϵCr = 5.62 ± 0.04, log ϵMn = 5.42 ± 0.04, log ϵFe = 7.47 ± 0.04, log ϵCo = 4.93 ± 0.05 and log ϵNi = 6.20 ± 0.04. Our uncertainties factor in both statistical and systematic errors (the latter estimated for possible errors in the model atmospheres and NLTE line formation). The new abundances are generally in good agreement with the CI meteoritic abundances but with some notable exceptions. This analysis constitutes both a full exposition and a slight update of the preliminary results we presented in Asplund et al. (2009, ARA&A, 47, 481), including full line lists and details of all input data we employed.
Key words: Sun: abundances / Sun: photosphere / Sun: granulation / line: formation / line: profiles / convection
Tables 1−3 are available in electronic form at http://www.aanda.org
© ESO, 2014
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