Численное моделирование развития неустойчивости медленной волны тонкой магнитной трубки в конвективной зоне Солнца

Magnetohydrodynamics of instability of thin magnetic tube within the limits of convective zone of the Sun is investigated in the paper. It is shown that slow wave instability is determining factor for the tube evolution. Slow wave instability leads to the strong changing of tube geometry, where the parts, which are emerging to the solar surface, and the parts, which are fixing near the bottom of convection zone, are segregated. Typical time of slow wave instability development can be significantly smaller, than the time of magnetic field confinement, which is found by calculations with use of one-dimensional models. The fixation of some tubes near the bottom of convection zone and the presence of differential rotation explicate the motion of the observed magnetic structures with respect to the sun surface.