Dust complexes form one of the Solar System components. There are many ways of their forming: ejection of matter from comets and satellites due to volcanic (geyser) eruptions and meteorites bombardement, explosions and collisions of artificial satellites, etc. Many works are dedicated to describe the distribution of matter in such complexes. In the present paper we find the shape of a typical complex under reasonable assumptions (the main one is the smallness of perturbations) using purely analytical methods.