  The model of a protoplanetary disk of a star with a low-mass companion
($M_2:M_1 \le 0.1$), moving on a circular orbit, which slightly inclined to the
disk plane ($\le 10^{\circ}$), is considered. The SPH-method is used to
calculate gas-dynamic ows. The motion of the companion on the orbit leads to
the inhomogeneous distribution of the matter in the disk: there are a cleared
gap, density waves and streams of matter. Because of the disturbances the inner
part of the disk is tilted to its periphery and also do not coincides with the
orbit plane of the companion. It leads to anisotropic illumination of the disk
by the star and, as a consequence, to the appearance of large-scale
inhomogeneity on the disk image: it has a bright area in the form of a
\horseshoe" and a small shadow zone located asymmetric with respect to the line
of nodes. The asymmetry of the disk image is clearly visible even if it is
observed pole-on. The motion of the companion on the orbit does not lead to the
synchronous movement of the shadow and bright areas: they only make small
oscillations relative to the some direction. By using the proposed model we an
fairly accurately reproduce the asymmetric image of the disk of star
LkH$\alpha$ 101, observed almost pole-on. The study of such asymmetric disks
opens up new opportunity for searching massive bodies around young stars.
