  To study the structure of spatially unresolved features of the solar
photosphere, we calculated the Stokes profiles of seven photospheric iron lines
using two-dimensional nonstationary MHD models of solar granulation for various
amounts of magnetic flux (0, 10, 20, 30 mT). We investigate variations in the
absolute wavelength shifts and bisectors of the I profiles, as well as
variations in the zero-crossing wavelength shifts, amplitude and area asymmetry
of the V profiles as functions of magnetic field strength and time. The
center-to-limb variations of the Stokes profiles are analyzed. The iron
abundance is found to be 7.57, with the photosphere inhomogeneities taken into
account. Although most of the spectral effects simulated within the scope of
the two-dimensional MHD models are in satisfactory agreement with observational
data, these models cannot always give a quantitative agreement. The absolute
wavelength shifts of the Stokes profiles of Fe II lines calculated with the MHD
models are substantially smaller than the observed ones.
