000001965 001__ 1965
000001965 005__ 20160701171656.0
000001965 0247_ $$2DOI$$a10.1051/0004-6361:20034328
000001965 037__ $$aASTROimport-122
000001965 100__ $$aAsplund, M.
000001965 245__ $$aLine formation in solar granulation. IV. [O I], O I and OH lines and the photospheric O abundance
000001965 260__ $$c2004
000001965 520__ $$aThe solar photospheric oxygen abundance has been determined from [O I], O I, OH vibration-rotation and OH pure rotation lines by means of a realistic time-dependent, 3D, hydrodynamical model of the solar atmosphere. In the case of the O I lines, 3D non-LTE calculations have been performed, revealing significant departures from LTE as a result of photon losses in the lines. We derive a solar oxygen abundance of log ɛO = 8.66 ± 0.05. All oxygen diagnostics yield highly consistent abundances, in sharp contrast with the results of classical 1D model atmospheres. This low value is in good agreement with measurements of the local interstellar medium and nearby B stars. This low abundance is also supported by the excellent correspondence between lines of very different line formation sensitivities, and between the observed and predicted line shapes and center-to-limb variations. Together with the corresponding down-ward revisions of the solar carbon, nitrogen and neon abundances, the resulting significant decrease in solar metal mass fraction to Z = 0.0126 can, however, potentially spoil the impressive agreement between predicted and observed sound speed in the solar interior determined from helioseismology. 
000001965 700__ $$a Grevesse, N.
000001965 700__ $$a Sauval, A. J.
000001965 700__ $$a Allende Prieto, C.
000001965 700__ $$a Kiselman, D.
000001965 773__ $$c751-768$$pAstronomy and Astrophysics$$v417$$y2004
000001965 85642 $$ahttp://esoads.eso.org/abs/2004A%26A...417..751A
000001965 905__ $$apublished in
000001965 980__ $$aREFERD