  Basic scenarios and mechanisms for the formation and decay of small-scale
magnetic elements and their manifestation in synthesized Stokes profiles of the
Fe I 15648.5 A infrared line are considered in the context of two-dimensional
modeling of nonstationary magnetogranulation on the Sun. The stage of
convective collapse is characterized by large redshifts in the V profiles
accompanied by complete Zeeman splitting of the I profiles. This is due to
intense downward flows of material, which facilitates the concentration of
longitudinal field with an amplitude of about several kG in the tube. The
dissipation of strong magnetic structures is characterized by blueshifts in the
Stokes profiles, which result from upward fluxes that decrease the magnetic
field in the tube. Typical signatures during key stages in the evolution of
compact magnetic elements should be detectable via observations with
sufficiently high spatial and temporal resolution.
