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We perform simulations of the dust and gas disk evolution to investigate theobservational features of a dust-pileup at the dead-zone inner edge. We showthat the total mass of accumulated dust particles is sensitive to theturbulence strength in the dead zone, $\alpha_{\rm dead}$, because of thecombined effect of turbulence-induced particle fragmentation (which suppressesparticle radial drift) and turbulent diffusion. For a typical criticalfragmentation velocity of silicate dust particles of $1~{\rm m~s^{-1}}$, thestress to pressure ratio $\alpha_{\rm dead}$ needs to be lower than $3 \times10^{-4}$ for dust trapping to operate. The obtained dust distribution ispostprocessed using the radiative transfer code RADMC-3D to simulate infraredscattered-light images of the inner part of protoplanetary disks with a dustpileup. We find that a dust pileup at the dead-zone inner edge, if present,casts a shadow extending out to $\sim 10~{\rm au}$. In the shadowed region thetemperature significantly drops, which in some cases yields even multiple watersnow lines. We also find that even without a dust pileup at the dead-zone inneredge, the disk surface can become thermally unstable, and the excited waves cannaturally produce shadows and ring-like structures in observed images. Thismechanism might account for the ring-like structures seen in thescattered-light images of some disks, such as the TW Hya disk.

Dust-Pileup at the Dead-Zone Inner Edge and Implications for the Disk Shadow