  Local three-dimensional shearing box simulations of the compressible coupled
dust-gas equations are used in the fluid approximation to study the evolution
of different initial vortex configurations in a protoplanetary disc and their
dust-trapping capabilities. The initial conditions for the gas are derived from
an analytic solution to the compressible Euler equation and the continuity
equation. The solution is valid if there is a vacuum outside the vortex. In the
simulations the vortex is either embedded in a hot corona, or it is extended in
a cylindrical fashion in the vertical direction. Both configurations are found
to survive for at least one orbit and lead to accumulation of dust inside the
vortex. This confirms earlier findings that dust accumulates in anticyclonic
vortices, indicating that this is a viable mechanism for planetesimal
formation.
