Elements with High First Ionization Potential in the New Chemical Composition of the Solar Photosphere

The responses of element abundances to the atmospheric model were statistically analyzed. The summarized 1998 data (1D models) and summarized 2009 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 the presence of regions in the photosphere where the temperature and magnetic field configuration favor fractionation of neutrals and ions. This, in turn, leads to a certain diffusion process similar to the coronal FIP effect. This type of diffusion is not taken into account in photospheric models. In this case, a new chemical composition of the Sun (3D) with decreased C, N, O and Ne abundances is appropriate only to narrow layers in the lower chromospheres (and possibly in the deep photosphere) and does not require revision of the standard solar model.