  A structure formed by dust particles ejected from the debris ring around HD
61005 is observed in the scattered light. The main aim here is to constrain
interstellar wind parameters that lead to shape morphology in the vicinity of
HD 61005 using currently available observational data for the debris ring.
Equation of motion of 2 $\times$ 10$^5$ dust particles ejected from the debris
ring under the action of the electromagnetic radiation, stellar wind, and
interstellar wind is solved. A two-dimensional (2D) grid is placed in a given
direction for accumulation of the light scattered on the dust particles in
order to determine the shape morphology. The interaction of the interstellar
wind and the stellar wind is considered. Groups of unknown properties of the
interstellar wind that create the observed morphology are determined. A
relation between number densities of gas components in the interstellar wind
and its relative velocity is found. Variations of the shape morphology caused
by the interaction with the interstellar clouds of various temperatures are
studied. When the interstellar wind velocity is tilted from debris ring axis a
simple relation between the properties of the interstellar wind and an angle
between the line of sight and the interstellar wind velocity exists. Dust
particles that are most significantly influenced by stellar radiation move on
the boundary of observed structure. Observed structure at HD 61005 can be
explained as a result of dust particles moving under the action of the
interstellar wind. Required number densities or velocities of the interstellar
wind are much higher than that of the interstellar wind entering the Solar
system.
