SIMBAD references

2017ApJ...843..150F - Astrophys. J., 843, 150-150 (2017/July-2)

A three-dimensional view of turbulence: constraints on turbulent motions In the HD 163296 protoplanetary disk using DCO+.

FLAHERTY K.M., HUGHES A.M., ROSE S.C., SIMON J.B., QI C., ANDREWS S.M., KOSPAL A., WILNER D.J., CHIANG E., ARMITAGE P.J. and BAI X.-N.

Abstract (from CDS):

Gas kinematics are an important part of the planet formation process. Turbulence influences planetesimal growth and migration from the scale of submicron 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), C18O(2-1) and CO(2-1)) from the disk around HD 163296. We are able to place stringent upper limits (vturb < 0.06cs, <0.05cs, and <0.04cs for CO(2-1), C18O(2-1), and DCO+(3-2) respectively), corresponding to α <= 3 x 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 magnetorotational instability and gravitoturbulence. In modeling the DCO+ emission, we also find that it is confined to three concentric rings at 65.7 ± 0.9 au, 149.9–0.7+0.5 au, and 259 ± 1 au, indicative of a complex chemical environment.

Abstract Copyright: © 2017. The American Astronomical Society. All rights reserved.

Journal keyword(s): accretion, accretion disks - protoplanetary disks - stars: individual: HD 163296 - turbulence - turbulence

Simbad objects: 6

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2019.12.07-12:47:28

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