  We study the vertical settling of solid bodies in a turbulent protoplanetary
disc. We consider the situation when the coupling to the gas is weak or
equivalently when the particle stopping time tau_{st} due to friction with the
gas is long compared to the orbital timescale Omega^{-1}. An analytical model,
which takes into account the stochastic nature of the sedimentation process
using a Fokker-Planck equation for the particle distribution function in phase
space, is used to obtain the vertical scale height of the solid layer as a
function of the vertical component of the turbulent gas velocity correlation
function and the particle stopping time. This is found to be of the same form
as the relation obtained for strongly coupled particles in previous work.
  We compare the predictions of this model with results obtained from local
shearing box MHD simulations of solid particles embedded in a vertically
stratified disc in which there is turbulence driven by the MRI. We find that
the ratio of the dust disc thickness to the gas disc thickness satifies
H_d/H=0.08 (Omega tau_{st})^{-1/2}, which is in very good agreement with the
analytical model. By discussing the conditions for gravitational instability in
the outer regions of protoplanetary discs in which there is a similar level of
turbulence, we find that bodies in the size range 50 to 600 metres can
aggregate to form Kuiper belt-like objects with characteristic radii ranging
from tens to hundreds of kilometres.
