Line formation in solar granulation III . The photospheric Si and meteoritic Fe abundances

@inproceedings{Asplund2000LineFI,
  title={Line formation in solar granulation III . The photospheric Si and meteoritic Fe abundances},
  author={M. S. Fredrik Asplund},
  year={2000}
}
Using realistic hydrodynamical simulations of the solar surface convection as 3D, time-dependent, inhomogeneous model atmospheres, the solar photospheric Si abundan ce has been determined to be log ǫSi = 7.51 ± 0.04. This constitutes a difference of 0.04 dex compared with previous estima tes based on the 1D Holweger-Müller (1974) model, of which half is attributable to the adopted model atmosphere and the rema ining part to the improved quantum mechanical broadening trea tment. As a consequence… CONTINUE READING
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