  X-ray- and extreme-ultraviolet- (XEUV-) driven photoevaporative winds acting
on protoplanetary disks around young T-Tauri stars may strongly impact disk
evolution, affecting both gas and dust distributions. We compute dust densities
for the wind regions of XEUV-irradiated transition disks with gap sizes of 20
and 30 AU, and determine whether they can be observed at wavelengths $0.7
\lesssim \lambda_\mathrm{obs} [\mu\mathrm{m}] \lesssim 1.8$ in scattered and
polarised light with current instrumentation. For an XEUV-driven outflow around
a $M_* = 0.7 \mathrm{M}_\odot$ T-Tauri star with $L_X = 2 \cdot 10^{30}
\mathrm{erg/s}$, we find dust mass-loss rates $\dot{M}_\mathrm{dust} \lesssim
2.0 \cdot 10^{-3} \dot{M}_\mathrm{gas}$, and if we invoke vertical settling,
the outflow is quite collimated. The synthesised images exhibit a distinct
chimney-like structure. The relative intensity of these chimneys is low, but
under optimal conditions, their detection may still be feasible with current
instrumentation such as JWST NIRCam and SPHERE IRDIS.
