Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 691, Issue 2, Pages L119-L122Publisher
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/691/2/L119
Keywords
line: formation; line: profiles; Sun: abundances; Sun: atmosphere; Sun: photosphere; techniques: polarimetric
Categories
Funding
- IAU Commission 46
- ANU
- Australian Research Council
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Determinations of the solar oxygen content relying on the neutral forbidden transition at 630 nm depend upon the nickel abundance, due to a Ni I blend. Here, we rederive the solar nickel abundance, using the same ab initio three-dimensional hydrodynamic model of the solar photosphere employed in the recent revision of the abundances of C, N, O, and other elements. Using 17 weak, unblended lines of Ni I together with the most accurate atomic and observational data available, we find log is an element of(Ni) = 6.17 +/- 0.02 ( statistical) +/- 0.05 ( systematic), a downward shift of 0.06-0.08 dex relative to previous abundances based on one-dimensional model atmospheres. We investigate the implications of the new nickel abundance for studies of the solar oxygen abundance based on the [O I] 630 nm line in the quiet Sun. Furthermore, we demonstrate that the oxygen abundance implied by the recent sunspot spectropolarimetric study of Centeno & Socas-Navarro needs to be revised downward from log is an element of(O) = 8.86 +/- 0.07 to 8.71 +/- 0.10. This revision is based on the new nickel abundance, the application of the best available gf value for the 630 nm forbidden oxygen line, and a more transparent treatment of CO formation. Determinations of the solar oxygen content relying on forbidden lines now appear to converge around log is an element of(O) = 8.7.
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