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

Abstract

We perform simulations of the dust and gas disk evolution to investigate the observational features of a dust-pileup at the dead-zone inner edge. We show that the total mass of accumulated dust particles is sensitive to the turbulence strength in the dead zone, ${\alpha }_{\mathrm{dead}}$, because of the combined effect of turbulence-induced particle fragmentation (which suppresses particle radial drift) and turbulent diffusion. For a typical critical fragmentation velocity of silicate dust particles of $1\mathrm{m}{\mathrm{s}}^{-1}$, the stress to pressure ratio ${\alpha }_{\mathrm{dead}}$ needs to be lower than $3\times 10^{-4}$ for dust trapping to operate. The obtained dust distribution is postprocessed using the radiative transfer code RADMC-3D to simulate infrared scattered-light images of the inner part of protoplanetary disks with a dust pileup. We find that a dust pileup at the dead-zone inner edge, if present, casts a shadow extending out to $\sim 10\mathrm{au}$. In the shadowed region the temperature significantly drops, which in some cases yields even multiple water snow lines. We also find that even without a dust pileup at the dead-zone inner edge, the disk surface can become thermally unstable, and the excited waves can naturally produce shadows and ring-like structures in observed images. This mechanism might account for the ring-like structures seen in the scattered-light images of some disks, such as the TW Hya disk.

arXiv comment16 pages, 13 figures, accepted for publication in ApJ

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