  We model the gas and dust dynamics in a turbulent protoplanetary disc
undergoing extreme-UV photoevaporation in order to better characterise the dust
properties in thermal winds (e.g. size distribution, flux rate, trajectories).
Our semi-analytic approach allows us to rapidly calculate these dust properties
without resorting to expensive hydrodynamic simulations. We find that
photoevaporation creates a vertical gas flow within the disc that assists
turbulence in supplying dust to the ionisation front. We examine both the
delivery of dust to the ionisation front and its subsequent entrainment in the
overlying wind. We derive a simple analytic criterion for the maximum grain
size that can be entrained and show that this is in good agreement with the
results of previous simulations where photoevaporation is driven by a range of
radiation types. We show that, in contrast to the case for magnetically driven
winds, we do not expect large scale dust transport within the disc to be
effected by photoevaporation. We also show that the maximum size of grains that
can be entrained in the wind ($s_{\rm max}$) is around an order of magnitude
larger than the maximum size of grains that can be delivered to the front by
advection alone ($s_{\rm crit} \lesssim 1$ $\mu{\rm m}$ for Herbig Ae/Be stars
and $\lesssim 0.01$ $\mu{\rm m}$ for T Tauri stars). We further investigate how
larger grains, up to a limiting size $s_{\rm limit}$, can be delivered to the
front by turbulent diffusion alone. In all cases, we find $s_{\rm max} \gtrsim
s_{\rm limit}$ so that we expect that any dust that is delivered to the front
can be entrained in the wind and that most entrained dust follows trajectories
close to that of the gas.
