  Among the candidates for generating turbulence in accretion discs in
situations with low intrinsic ionization the vertical shear instability (VSI)
has become an interesting candidate, as it relies purely on a vertical gradient
in the angular velocity. Existing simulations have shown that $\alpha$-values a
few times $10^{-4}$ can be generated. The particle growth in the early planet
formation phase is determined by the dynamics of dust particles. Here, we
address in particular the efficiency of VSI-turbulence in concentrating
particles in order to generate overdensities and low collision velocities. We
perform 3D numerical hydrodynamical simulations of accretion discs around young
stars that include radiative transport and irradiation from the central star.
The motion of particles within a size range of a fraction of mm up to several m
is followed using standard drag formula. We confirm that under realistic
conditions the VSI is able to generate turbulence in full 3D protoplanetary
discs. The irradiated disc shows turbulence within 10 to 60au. The mean radial
motion of the gas is such that it is directed inward near the midplane and
outward in the surface layers. We find that large particles drift inward with
the expected speed, while small particles can experience phases of outward
drift. Additionally, the particles show bunching behaviour with overdensities
reaching 5 times the average value, which is strongest for dimensionless
stopping times around unity. Particles in a VSI-turbulent discs are
concentrated in large scale turbulent eddies and show low relative speeds that
allow for growing collisions. The reached overdensities will also allow for the
onset streaming instabilities further enhancing particle growth. The outward
drift for small particles at higher disk elevations allows for the transport of
processed high temperature material in the Solar System to larger distances.
