Dust entrainment in photoevaporative winds: Synthetic observations of transition disks

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