Elements with high first ionization potential in new chemical composition of the Solar photosphere

The statistical analysis of responses of element abundances to the atmospheric model was made. The 1998 summarized data (1D models) and 2009 summarized data (3D models) were compared. A significant statistical dependence between the response value and the first ionization potential (FIP) of an element was shown. This phenomenon may be caused by presence of regions in the photosphere where the temperature and magnetic field configuration favour fractionation of neutrals and ions; this, in its turn, leads to a certain diffusion process similar to the coronal FIP effect. This type of diffusion is not taken into account in photosphere models. In this case, a new chemical composition of the Sun (3D) with lowered C, N, O and Ne abundances is appropriate only to narrow layers in the lower chromosphere (and possibly in the deep photosphere) and does not require revision of the standard solar model.