Dust entrainment in photoevaporative winds: The impact of X-rays

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{e}\mathrm{r}\mathrm{g}\mathrm{/}\mathrm{s}$$emittedbya$M_* = 0.7,$\mathrm{M}$\odot$ star, corresponding to a wind mass-loss rate of $\dot{M}$\mathrm{w}$ \simeq 2.6 \cdot 10^{-8} ,${\mathrm{M}}_{\odot }\mathrm{/}\mathrm{y}\mathrm{r}$$,wefinddustentrainmentforsizes$a_0 \lesssim 11,\mu$m($9,\mu$m)fromtheinner$25,$AU($120,$AU). This is an enhancement over dust entrainment in less vigorous EUV-driven winds with ${\dot{M}}_{\mathrm{w}}\simeq {10}^{-10}{\mathrm{M}}_{\odot }\mathrm{/}\mathrm{y}\mathrm{r}$. 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.