Evolution of solar magnetic tubes from observations of Stokes parameters

Basic scenarios and mechanisms for the formation and decay of small-scale m agnetic elements and their manifestation in synthesized Stokes profiles of the Fe I 15648.5 Angstrom infrared line are considered in the context of tw o-dimensional modeling of nonstationary magnetogranulation on the Sun. The stage of convective collapse is characterized by large redshifts in the Ir profiles accompanied by complete Zeeman splitting of the I profiles. This i s due to intense downward flows of material, which facilitates the concentr ation of longitudinal field with an amplitude of about several kG in the tu be. The dissipation of strong magnetic structures is characterized by blues hifts in their profiles, which result from upward fluxes that decrease the magnetic field in the tube. Typical signatures during key stages in the evo lution of compact magnetic elements should be detectable via observations w ith sufficiently high spatial and temporal resolution. (C) 2000 MAIK "Nauka /Interperiodica".