A major asymmetric ice trap in a planet-forming disk

Booth, Alice S.; Marel, Nienke van der; Leemker, M.; Dishoeck, E. F. van; Ohashi, Satoshi

doi:10.1051/0004-6361/202141057

Cited by 34 publications

(36 citation statements)

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“…Considering the reported rms level of 1.2 mJy bm −1 channel −1 with a channel width of 1.6 km s −1 , a line width of ∼14 km s −1 and a beam size of 0.63×0.50" (van der Marel et al 2021), we compute a 3σ upper limit on the C 2 H flux density of 11 mJy bm −1 km s −1 , or a scaled T b,peak,100pc limit of <1.1 K km s −1 . Such a low value of C 2 H is consistent with the low CS/SO ratio reported by Booth et al (2021a).…”

Section: Appendix A: Icy Dust Mass Calculationsupporting

confidence: 91%

“…Current disk surveys of C/O tracers such as C 2 H (Bergin et al 2016;Semenov et al 2018;Cleeves et al 2018) appear to show a bimodal distribution of disks with and without C 2 H detection indicating either high (C/O>1) or low (C/O<1) ratios (Bergner et al 2019;Miotello et al 2019) but it is unclear whether this bimodality is an intrinsic property or the result of physical-chemical processes. The recent discovery of low C/O at the location of the asymmetric Oph IRS 48 dust trap (Booth et al 2021a) suggests that pressure bumps may play a key role in regulating the C/O profile in disks, which is particularly relevant considering that pressure bumps are usually associated with giant planets (e.g. Pinilla et al 2012b;van der Marel et al 2016) and those planets would accrete the composition of the gaseous material at the bump location.…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Appendix A: Icy Dust Mass Calculationsupporting

confidence: 91%

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

Self Cite

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“…The emission from these regions may also be related to the action of inner jets and outflow (e.g., Podio et al 2021) or to the innermost regions of disk and envelope (e.g., Harsono et al 2021) where dust mantles can sublimate, thus resembling a hot-corino chemistry. Booth et al (2021) also showed an asymmetric SO and SO 2 emission co-spatial with a dust crescent where the molecular enhancement would be related to the sublimation of ices at the edge of a dust cavity at a separation of ∼50 au. However, in the case of HL Tau presented here, a further explanation is possible.…”

Section: Origin Of the So And So 2 Emissionmentioning

confidence: 90%

ALMA chemical survey of disk-outflow sources in Taurus (ALMA-DOT)

Garufi

Podio

Codella

et al. 2022

A&A

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Planet-forming disks are not isolated systems. Their interaction with the surrounding medium affects their mass budget and chemical content. In the context of the ALMA-DOT program, we obtained high-resolution maps of assorted lines from six disks that are still partly embedded in their natal envelope. In this work, we examine the SO and SO2 emission that is detected from four sources: DG Tau, HL Tau, IRAS 04302+2247, and T Tau. The comparison with CO, HCO+, and CS maps reveals that the SO and SO2 emission originates at the intersection between extended streamers and the planet-forming disk. Two targets, DG Tau and HL Tau, offer clear cases of inflowing material inducing an accretion shock on the disk material. The measured rotational temperatures and radial velocities are consistent with this view. In contrast to younger Class 0 sources, these shocks are confined to the specific disk region impacted by the streamer. In HL Tau, the known accreting streamer induces a shock in the disk outskirts, and the released SO and SO2 molecules spiral toward the star in a few hundred years. These results suggest that shocks induced by late accreting material may be common in the disks of young star-forming regions with possible consequences for the chemical composition and mass content of the disk. They also highlight the importance of SO and SO2 line observations in probing accretion shocks from a larger sample.

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“…We note that H 2 CS was detected in MWC 480 (Le Gal et al 2019), and H 2 S was detected in GG Tau (Phuong et al 2018) and in four protoplanetary disks in Taurus (Rivière-Marichalar et al 2021). Furthermore, SO has been detected in a few PPDs (Pacheco-Vázquez et al 2016;Booth et al 2018Booth et al , 2021Le Gal et al 2021), and SO 2 has been observed toward IRS 48 as well (Booth et al 2021). Recently, CCS was detected toward GG Tau (Phuong et al 2021), but the low signal-to-noise ratio (s/n) precluded the analysis of the spatial distribution.…”

Section: Introductionmentioning

confidence: 99%

AB Aur, a Rosetta stone for studies of planet formation

Riviére-Marichalar

Fuente

Esplugues

et al. 2022

A&A

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Context. The sulfur abundance is poorly known in most environments. Yet, deriving the sulfur abundance is key to understanding the evolution of the chemistry from molecular clouds to planetary atmospheres. We present observations of H 2 S 1 10 − 1 01 at 168.763 GHz toward the Herbig Ae star AB Aur. Aims. We aim to study the abundance of sulfuretted species toward AB Aur and to constrain how different species and phases contribute to the sulfur budget. Methods. We present new NOrthern Extended Millimeter Array (NOEMA) interferometric observations of the continuum and H 2 S 1 10 − 1 01 line at 168.763 GHz toward AB Aur. We derived radial and azimuthal profiles and used them to compare the geometrical distribution of different species in the disk. Assuming local thermodynamical equilibrium (LTE), we derived column density and abundance maps for H 2 S, and we further used Nautilus to produce a more detailed model of the chemical abundances at different heights over the mid-plane at a distance of r=200 au. Results. We have resolved H 2 S emission in the AB Aur protoplanetary disk. The emission comes from a ring extending from 0.67 (∼109 au) to 1.69 (∼275 au). Assuming T=30 K, n H =10 9 cm −3 , and an ortho-to-para ratio of three, we derived a column density of (2.3±0.5)×10 13 cm −2 . Under simple assumptions, we derived an abundance of (3.1±0.8)×10 −10 with respect to H nuclei, which we compare with Nautilus models to deepen our understanding of the sulfur chemistry in protoplanetary disks. Chemical models indicate that H 2 S is an important sulfur carrier in the solid and gas phase. We also find an important transition at a height of ∼12 au, where the sulfur budget moves from being dominated by ice species to being dominated by gas species. Conclusions. We confirm that present-day models still struggle to simultaneously reproduce the observed column densities of the different sulfuretted species, and the observed abundances are still orders of magnitude away from the cosmic sulfur abundance. Studying sulfuretted species in detail in the different phases of theinterstellar medium is key to solving the issue.

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A major asymmetric ice trap in a planet-forming disk

Cited by 34 publications

References 58 publications

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

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

ALMA chemical survey of disk-outflow sources in Taurus (ALMA-DOT)

AB Aur, a Rosetta stone for studies of planet formation

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