  The particle dynamics of the recently observed ring around dwarf planet
Haumea is numerically investigated. The point mass gravitational force, a
second degree and order gravity field, and the solar radiation pressure as the
main perturbations are considered. The quasi-stationary state of the ring
varies for different micron-sized grains and depends also on the spin-orbit
resonances between the rotation rate of the main body and the orbital period of
the dust particles. The simulations confirm the variable radial width of the
ring observed during the transit ingress and egress. Results show that the
micron sized grains, initially on circular orbits, become eccentric and form an
apse-aligned ring at the observed radial distance near to the 3:1 spin-orbit
resonance. It is also demonstrated that this coincidence is only apparent and
independent of 3:1 resonance.
