Line Formation in Solar Granulation: IV.[OI], OI and OH Lines and The
Astronomy & Astrophysics manuscript no. 0328 March 17, 2018 (DOI: will be inserted by hand later) Line formation in solar granulation IV. [O I], O I and OH lines and the photospheric O abundance Martin Asplund1, Nicolas Grevesse2,3, A. Jacques Sauval4, Carlos Allende Prieto5 and Dan Kiselman6 1 Research School of Astronomy and Astrophysics, Mt. Stromlo Observatory, Cotter Rd., Weston, ACT 2611, Australia 2 Centre Spatial de Li`ege, Universit´ede Li`ege, avenue Pr´e Aily, B-4031 Angleur-Li`ege, Belgium 3 Institut d’Astrophysique et de G´eophysique, Universit´e de Li`ege, All´ee du 6 aoˆut, 17, B5C, B-4000 Li`ege, Belgium 4 Observatoire Royal de Belgique, avenue circulaire, 3, B-1180 Bruxelles, Belgium 5 McDonald Observatory and Department of Astronomy, University of Texas, Austin, TX 78712-1083, USA 6 The Institute for Solar Physics of the Royal Swedish Academy of Sciences, AlbaNova University Centre, SE-106 91 Stockholm, Sweden Accepted for Astronomy & Astrophysics Abstract. The 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 ǫO = 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.
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