Context : 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 .

Aims : We investigate the dust entrainment in XEUV-driven photoevaporative winds and compare our results to existing MHD and EUV-only models .

Methods : We used a 2D hydrodynamical gas model of a protoplanetary disk irradiated by both X-ray and EUV spectra from a central T-Tauri star to trace the motion of passive Lagrangian dust grains of various sizes .
The trajectories were modelled starting at the disk surface in order to investigate dust entrainment in the wind .

Results : 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 .

Conclusions : X-ray-driven photoevaporative winds are expected to be dust-rich if small grains are present in the disk atmosphere .