Dust growth, fragmentation and self-induced dust traps in PHANTOM

Vericel, Arnaud; Gonzalez, Jean-François; Price, Daniel J.; Laibe, Guillaume; Pinte, Christophe

doi:10.48550/arxiv.2108.00878

Cited by 1 publication

(1 citation statement)

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“…In this manuscript the term dust ring and pressure bump are used interchangeably, although dust rings without pressure bumps may also exist (e.g. Okuzumi et al 2016;Vericel et al 2021). The samples of the C 2 H surveys by Bergner et al (2019); Miotello et al (2019) are biased towards brighter millimeter continuum disks, which are known to contain pressure bumps more often (Pinilla et al 2020;van der Marel & Mulders 2021), as either ring disks (Andrews et al 2018, e.g.…”

Section: Introductionmentioning

confidence: 99%

If you like C/O variations, you should have put a ring on it

van der Marel,

Bosman,

Krijt

et al. 2021

Preprint

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Context. The C/O-ratio as traced with C 2 H emission in protoplanetary disks is fundamental for constraining the formation mechanisms of exoplanets and our understanding of volatile depletion in disks, but current C 2 H observations show an apparent bimodal distribution which is not well understood, indicating that the C/O distribution is not described by a simple radial dependence. Aims. The transport of icy pebbles has been suggested to alter the local elemental abundances in protoplanetary disks, through settling, drift and trapping in pressure bumps resulting in a depletion of volatiles in the surface and an increase of the elemental C/O. Methods. We combine all disks with spatially resolved ALMA C 2 H observations with high-resolution continuum images and constraints on the CO snowline to determine if the C 2 H emission is indeed related to the location of the icy pebbles. Results. We report a possible correlation between the presence of a significant CO-icy dust reservoir and high C 2 H emission, which is only found in disks with dust rings outside the CO snowline. In contrast, compact dust disks (without pressure bumps) and warm transition disks (with their dust ring inside the CO snowline) are not detected in C 2 H, suggesting that such disks may never have contained a significant CO ice reservoir. Conclusions. This correlation provides evidence for the regulation of the C/O profile by the complex interplay of CO snowline and pressure bump locations in the disk. These results demonstrate the importance of including dust transport in chemical disk models, for a proper interpretation of exoplanet atmospheric compositions, and a better understanding of volatile depletion in disks, in particular the use of CO isotopologues to determine gas surface densities.

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