  The motion of planetesimals initially located in the feeding zone of the
planet Proxima Centauri c, at distances of 500 AU from the star to the star's
Hill sphere radius of 1200 AU was considered. In the analyzed non-gaseous
model, the primary ejection of planetesimals from most of the feeding zone of
an almost formed planet c to distances greater than 500 AU from the star
occurred during the first 10 million years. Only for planetesimals originally
located at the edges of the planet's feeding zone, the fraction of
planetesimals that first reached 500 AU over the time greater than 10 million
years was more than half. Some planetesimals could reach the outer part of the
star's Hill sphere over hundreds of millions of years. Most of the
planetesimals that first reached 500 AU from Proxima Centauri first reached
1200 AU from the star in less than 1 million years. In the considered model,
the disk of planetesimals in the outer part of the star's Hill sphere was
rather flat. The results may be of interest for understanding the motion of
bodies in other exoplanetary systems, especially those with a single dominant
planet. The strongly inclined orbits of bodies in the outer part of Proxima
Centauri's Hill sphere can primarily result from bodies that entered the Hill
sphere from outside. The radius of Proxima Centauri's Hill sphere is an order
of magnitude smaller than the radius of the outer boundary of the Hills cloud
in the Solar System and two orders of magnitude smaller than the radius of the
Sun's Hill sphere. Therefore, it is difficult to expect the existence of a
similarly massive cloud around this star as the Oort cloud around the Sun.
