A Three-Dimensional View of Turbulence: Constraints on Turbulent Motions in the HD 163296 Protoplanetary Disk using DCO${}^{+}$

Abstract

Gas kinematics are an important part of the planet formation process. Turbulence influences planetesimal growth and migration from the scale of sub-micron dust grains through gas-giant planets. Radio observations of resolved molecular line emission can directly measure this non-thermal motion and, taking advantage of the layered chemical structure of disks, different molecular lines can be combined to map the turbulence throughout the vertical extent of a protoplanetary disk. Here we present ALMA observations of three molecules (DCO${}^{+}$(3-2), C${}^{18}$O(2-1) and CO(2-1)) from the disk around HD 163296. We are able to place stringent upper limits ($v_{\mathrm{turb}}<$0.06c${}_s$, $<$0.05c${}_s$ and $<$0.04c${}_s$ for CO(2-1), C${}^{18}$O(2-1) and DCO${}^{+}$(3-2) respectively), corresponding to $\alpha \lesssim$3$\times$10${}^{-3}$, similar to our prior limit derived from CO(3-2). This indicates that there is little turbulence throughout the vertical extent of the disk, contrary to theoretical predictions based on the magneto-rotational instability and gravito-turbulence. In modeling the DCO${}^{+}$ emission we also find that it is confined to three concentric rings at 65.7$\pm$0.9 au, 149.9${}_{-0.7}^{+0.5}$ au and 259$\pm$1 au, indicative of a complex chemical environment.

Accepted to ApJ

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