  Using realistic hydrodynamical simulations of the solar surface convection as
3D, time-dependent, inhomogeneous model atmospheres, the solar photospheric Si
abundance has been determined to be log Si = 7.51 +- 0.04. This constitutes a
difference of 0.04 dex compared with previous estimates based on the 1D
Holweger-M\"uller (1974) model, of which half is attributable to the adopted
model atmosphere and the remaining part to the improved quantum mechanical
broadening treatment. As a consequence, all meteoritic abundances should be
adjusted downwards by the same amount. In particular the meteoritic Fe
abundance will be log Fe = 7.46 +- 0.01, in good agreement with the recently
determined photospheric Fe abundance (Asplund et al. 2000b). The existing
uncertainties unfortunately prevent an observational confirmation of the
postulated effects of elemental migration of metals in the Sun.
