A major asymmetric ice trap in a planet-forming disk

Brunken, N. G. C.; Booth, Alice S.; Leemker, M.; Nazari, P.; Marel, Nienke van der; Dishoeck, E. F. van

doi:10.1051/0004-6361/202142981

Cited by 37 publications

(30 citation statements)

References 49 publications

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“…Most strikingly, in the IRS 48 disk, multiple different molecules clearly follow the millimeter dust distribution. IRS 48 shows a clear chemical asymmetry: The sulphur monoxide (SO), sulphur dioxide (SO 2 ), nitric oxide (NO), formaldehyde (H 2 CO), methanol (CH 3 OH), and dimethyl ether (CH 3 OCH 3 ) are all co-spatial with the highly asymmetric dust trap (van der Marel et al 2021b;Booth et al 2021a;Brunken et al 2022). The most likely chemical origin of these species is thermal sublimation of H 2 O and more complex organic ices at the edge of the irradiated dust cavity.…”

Section: Introductionmentioning

confidence: 99%

Sulphur monoxide emission tracing an embedded planet in the HD 100546 protoplanetary disk

Booth

Ilee

Walsh

et al. 2023

A&A

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Molecular line observations are powerful tracers of the physical and chemical conditions across the different evolutionary stages of star, disk, and planet formation. The high angular resolution and unprecedented sensitivity of the Atacama Large Millimeter Array (ALMA) enables the current drive to detect small-scale gas structures in protoplanetary disks that can be attributed directly to forming planets. We report high angular resolution ALMA Band 7 observations of sulphur monoxide (SO) in the nearby planet-hosting disk around the Herbig star HD 100546. SO is rarely detected in evolved protoplanetary disks, but in other environments, it is most often used as a tracer of shocks. The SO emission from the HD 100546 disk primarily originates from gas within the ≈20 au millimeterdust cavity and shows a clear azimuthal brightness asymmetry of a factor of 2. In addition, the difference in the line profile shape is significant when these new Cycle 7 data are compared to Cycle 0 data of the same SO transitions. We discuss the different physical and chemical mechanisms that might cause this asymmetry and time variability, including disk winds, disk warps, and a shock triggered by a (forming) planet. We propose that SO is enhanced in the cavity by the presence of a giant planet. The SO asymmetry complements evidence for hot circumplanetary material around giant planet HD 100546 c that is traced via CO ro-vibrational emission. This work sets the stage for further observational and modelling efforts to detect and understand the chemical imprint of a forming planet on its parent disk.

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Section: Introductionmentioning

confidence: 99%

Sulphur monoxide emission tracing an embedded planet in the HD 100546 protoplanetary disk

Booth

Ilee

Walsh

et al. 2023

A&A

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“…At that stage, ices are exposed to radiation from cosmic rays and the YSO and residue formation is expected to take place. A fraction of the interstellar ices and organic residues is transferred to the protoplanetary disk , and becomes incorporated into meteorite parent bodies, which then undergo aqueous alteration at various temperatures. − Temperatures of 50 and 125 °C and relatively short heating time scales were chosen for the experiments to reflect the processes in parent bodies that contain CI, CM, and CR chondrites and may account for the extended periods of time (∼10 4 –10 6 years) when liquid water was present in the parent body, because they exhibit only moderate degrees of aqueous alteration. − Additionally, an experimental heating time scale that includes 2–30 days has been reported in the literature, , and therefore, the chemical changes observed in this study can be compared to that of related studies.…”

Section: Introductionmentioning

confidence: 99%

Meteorite Parent Body Aqueous Alteration Simulations of Interstellar Residue Analogs

Qasim

Aponte

Glavin

et al. 2023

ACS Earth Space Chem.

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Some families of carbonaceous chondrites are rich in prebiotic organics that may have contributed to the origin of life on Earth and elsewhere. However, the formation and chemical evolution of complex soluble organic molecules from interstellar precursors under relevant parent body conditions has not been thoroughly investigated. In this study, we approach this topic by simulating meteorite parent body aqueous alteration of interstellar residue analogs. The distributions of amines and amino acids are qualitatively and quantitatively investigated and linked to closing the gap between interstellar and meteoritic prebiotic organic abundances. We find that the abundance trend of methylamine > ethylamine> glycine > serine > alanine > β-alanine does not change from pre-to post-aqueous alteration, suggesting that certain parental cloud conditions have an influential role on the distributions of interstellar-inherited meteoritic organics. However, the abundances for most of the amines and amino acids studied here varied by about 2-fold when aqueously processed for 7 days at 125 °C, and the changes in the αto β-alanine ratio were consistent with those of aqueously altered carbonaceous chondrites, pointing to an influential role of meteorite parent body processing on the distributions of interstellar-inherited meteoritic organics. We detected higher abundances of αover β-alanine, which is opposite to what is typically observed in aqueously altered carbonaceous chondrites; these results may be explained by at least the lack of minerals, inorganic species, and insoluble organic matter-relevant materials in the experiments. The high abundance of volatile amines in the non-aqueously altered samples suggests that these types of interstellar volatiles can be efficiently transferred to asteroids and comets, supporting the idea of the presence of interstellar organics in solar system objects.

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“…They discussed that at the inner edge, CH 3 OH is proposed to originate from thermal desorption. van der Marel et al (2021) and Brunken et al (2022) reported the detections of CH 3 OH, H 2 CO, and CH 3 OCH 3 line emission in the vicinity of the asymmetric dust trap in the disk around a Herbig Ae star Oph IRS 48 (see also Booth et al 2021b). They discussed that these molecules are thermally desorbed from icy dust grains and that such dust traps provide huge icy grain reservoirs in the disk midplane.…”

Section: Implication For the Observations Of Protoplanetary Disksmentioning

confidence: 99%

The Molecular Composition of Shadowed Proto-solar Disk Midplanes Beyond the Water Snowline

Notsu

Ohno

Ueda

et al. 2022

ApJ

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The disk midplane temperature is potentially affected by the dust traps/rings. The dust depletion beyond the water snowline will cast a shadow. In this study, we adopt a detailed gas-grain chemical reaction network, and investigate the radial gas and ice abundance distributions of dominant carbon-, oxygen-, and nitrogen-bearing molecules in disks with shadow structures beyond the water snowline around a proto-solar-like star. In shadowed disks, the dust grains at r ∼ 3–8 au are predicted to have more than ∼5–10 times the amount of ices of organic molecules such as H2CO, CH3OH, and NH2CHO, saturated hydrocarbon ices such as CH4 and C2H6, in addition to H2O, CO, CO2, NH3, N2, and HCN ices, compared with those in non-shadowed disks. In the shadowed regions, we find that hydrogenation (especially of CO ice) is the dominant formation mechanism of complex organic molecules. The gas-phase N/O ratios show much larger spatial variations than the gas-phase C/O ratios; thus, the N/O ratio is predicted to be a useful tracer of the shadowed region. N2H+ line emission is a potential tracer of the shadowed region. We conclude that a shadowed region allows for the recondensation of key volatiles onto dust grains, provides a region of chemical enrichment of ices that is much closer to the star than within a non-shadowed disk, and may explain to some degree the trapping of O2 ice in dust grains that formed comet 67P/Churyumov-Gerasimenko. We discuss that, if formed in a shadowed disk, Jupiter does not need to have migrated vast distances.

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A major asymmetric ice trap in a planet-forming disk

Cited by 37 publications

References 49 publications

Sulphur monoxide emission tracing an embedded planet in the HD 100546 protoplanetary disk

Sulphur monoxide emission tracing an embedded planet in the HD 100546 protoplanetary disk

Meteorite Parent Body Aqueous Alteration Simulations of Interstellar Residue Analogs

The Molecular Composition of Shadowed Proto-solar Disk Midplanes Beyond the Water Snowline

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