  X-ray- and EUV- (XEUV-) driven photoevaporative winds acting on
protoplanetary disks around young T-Tauri stars may crucially impact disk
evolution, affecting both gas and dust distributions. We investigate the dust
entrainment in XEUV-driven photoevaporative winds and compare our results to
existing MHD and EUV-only models. For an X-ray luminosity of $L_X = 2 \cdot
10^{30}\,\mathrm{erg/s}$ emitted by a $M_* = 0.7\,\mathrm{M}_\odot$ star,
corresponding to a wind mass-loss rate of $\dot{M}_\mathrm{w} \simeq 2.6 \cdot
10^{-8} \,\mathrm{M_\odot/yr}$, we find dust entrainment for sizes $a_0
\lesssim 11\,\mu$m ($9\,\mu$m) from the inner $25\,$AU ($120\,$AU). This is an
enhancement over dust entrainment in less vigorous EUV-driven winds with
$\dot{M}_\mathrm{w} \simeq 10^{-10}\,\mathrm{M_\odot/yr}$. Our numerical model
also shows deviations of dust grain trajectories from the gas streamlines even
for $\mu$m-sized particles. In addition, we find a correlation between the size
of the entrained grains and the maximum height they reach in the outflow.
