Line formation in solar granulation

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 . 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…

• NS
  National Science Foundation

  Award: 0086321
• NA
  National Aeronautics and Space Administration
• GG
  Göran Gustafssons Stiftelser
• RS
  Royal Swedish Academy of Sciences
• ID
  Instituto de Astrofísica de Canarias
• AR
  Australian Research Council