The Disk Substructures at High Angular Resolution Project (DSHARP): II. Characteristics of Annular Substructures. (arXiv:1812.04041v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Huang_J/0/1/0/all/0/1">Jane Huang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Andrews_S/0/1/0/all/0/1">Sean M. Andrews</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dullemond_C/0/1/0/all/0/1">Cornelis P. Dullemond</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Isella_A/0/1/0/all/0/1">Andrea Isella</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Perez_L/0/1/0/all/0/1">Laura M. Pérez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guzman_V/0/1/0/all/0/1">Viviana V. Guzmán</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+%7FOberg_K/0/1/0/all/0/1">Karin I. Öberg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhu_Z/0/1/0/all/0/1">Zhaohuan Zhu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_S/0/1/0/all/0/1">Shangjia Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bai_X/0/1/0/all/0/1">Xue-Ning Bai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benisty_M/0/1/0/all/0/1">Myriam Benisty</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Birnstiel_T/0/1/0/all/0/1">Tilman Birnstiel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carpenter_J/0/1/0/all/0/1">John M. Carpenter</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hughes_A/0/1/0/all/0/1">A. Meredith Hughes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ricci_L/0/1/0/all/0/1">Luca Ricci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Weaver_E/0/1/0/all/0/1">Erik Weaver</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wilner_D/0/1/0/all/0/1">David J. Wilner</a>
The Disk Substructures at High Angular Resolution Project used ALMA to map
the 1.25 millimeter continuum of protoplanetary disks at a spatial resolution
of ~5 au (Andrews et al. 2018a). We present a systematic analysis of annular
substructures in the 18 single-disk systems targeted in this survey. No
dominant architecture emerges from this sample; instead, remarkably diverse
morphologies are observed. Annular substructures can occur at virtually any
radius where millimeter continuum emission is detected and range in widths from
a few au to tens of au. Intensity ratios between gaps and adjacent rings range
from near-unity to just a few percent. In a minority of cases, annular
substructures co-exist with other types of substructures, including spiral arms
(3/18) and crescent-like azimuthal asymmetries (2/18). No clear trend is
observed between the positions of the substructures and stellar host
properties. In particular, the absence of an obvious association with stellar
host luminosity (and hence the disk thermal structure) suggests that
substructures do not occur preferentially near major molecular snowlines.
Annular substructures like those observed in DSHARP have long been hypothesized
to be due to planet-disk interactions. A few disks exhibit characteristics
particularly suggestive of this scenario, including substructures in possible
mean-motion resonance and “double gap” features reminiscent of hydrodynamical
simulations of multiple gaps opened by a planet in a low-viscosity disk.
The Disk Substructures at High Angular Resolution Project used ALMA to map
the 1.25 millimeter continuum of protoplanetary disks at a spatial resolution
of ~5 au (Andrews et al. 2018a). We present a systematic analysis of annular
substructures in the 18 single-disk systems targeted in this survey. No
dominant architecture emerges from this sample; instead, remarkably diverse
morphologies are observed. Annular substructures can occur at virtually any
radius where millimeter continuum emission is detected and range in widths from
a few au to tens of au. Intensity ratios between gaps and adjacent rings range
from near-unity to just a few percent. In a minority of cases, annular
substructures co-exist with other types of substructures, including spiral arms
(3/18) and crescent-like azimuthal asymmetries (2/18). No clear trend is
observed between the positions of the substructures and stellar host
properties. In particular, the absence of an obvious association with stellar
host luminosity (and hence the disk thermal structure) suggests that
substructures do not occur preferentially near major molecular snowlines.
Annular substructures like those observed in DSHARP have long been hypothesized
to be due to planet-disk interactions. A few disks exhibit characteristics
particularly suggestive of this scenario, including substructures in possible
mean-motion resonance and “double gap” features reminiscent of hydrodynamical
simulations of multiple gaps opened by a planet in a low-viscosity disk.
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