Динамика пылинок и малых тел в аккреционных дисках молодых звезд с остаточным магнитным полем

The paper presents a numerical model of the dynamics of dust particles and small bodies in accretion disks with fossil magnetic field. The model equations include gravity, centrifugal force, and gas drag force. The disk structure is simulated using the magnetohydrodynamic model of Dudorov and Khaibrakhmanov taking into account the effect of magnetic tensions on the gas rotation velocity. The results show that 1 m-sized particles quickly settle on the midplane, experiencing damped oscillations, and then slowly drift toward the star. Magnetic tensions increase the radial drift velocity at the disk periphery, accelerating the process of depletion of solid particles in the outer regions and their accumulation in 'dead' zones.