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000002314 0247_ $$2DOI$$a10.1146/annurev.astro.46.060407.145222
000002314 037__ $$aASTROimport-471
000002314 100__ $$aAsplund, M.
000002314 245__ $$aThe Chemical Composition of the Sun
000002314 260__ $$c2009
000002314 520__ $$aThe solar chemical composition is an important ingredient in our understanding of the formation, structure, and evolution of both the Sun and our Solar System. Furthermore, it is an essential reference standard against which the elemental contents of other astronomical objects are compared. In this review, we evaluate the current understanding of the solar photospheric composition. In particular, we present a redetermination of the abundances of nearly all available elements, using a realistic new three-dimensional (3D), time-dependent hydrodynamical model of the solar atmosphere. We have carefully considered the atomic input data and selection of spectral lines, and accounted for departures from local thermodynamic equilibrium (LTE) whenever possible. The end result is a comprehensive and homogeneous compilation of the solar elemental abundances. Particularly noteworthy findings are significantly lower abundances of C, N, O, and Ne compared to the widely used values of a decade ago. The new solar chemical composition is supported by a high degree of internal consistency between available abundance indicators, and by agreement with values obtained in the Solar Neighborhood and from the most pristine meteorites. There is, however, a stark conflict with standard models of the solar interior according to helioseismology, a discrepancy that has yet to find a satisfactory resolution. 
000002314 700__ $$a Grevesse, N.
000002314 700__ $$a Sauval, A. J.
000002314 700__ $$a Scott, P.
000002314 773__ $$c481-522$$i1$$pAnnual Review of Astronomy and Astrophysics$$v47$$y2009
000002314 85642 $$ahttp://esoads.eso.org/abs/2009ARA%26A..47..481A
000002314 905__ $$apublished in
000002314 980__ $$aREFERD