Tracing pebble drift and trapping using radial carbon depletion profiles in protoplanetary disks

Sturm, J. A.; McClure, M. K.; Harsono, D.; Facchini, S.; Long, F.; Kama, M.; Bergin, E. A.; van Dishoeck, E. F.

doi:10.48550/arxiv.2201.04089

Cited by 4 publications

(6 citation statements)

References 84 publications

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“…Interestingly enough, the CO-HD discrepancy is not there for warmer disks around Herbig stars (Kama et al 2020), supporting the idea of volatile lock-up happening when freeze-out is more efficient. A similar trend between C depletion and disk temperature has been recently found with [CI] Atacama Compact Array (ACA) observations by Sturm et al (2022).…”

Section: Gas Mass From Hd Emission -supporting

confidence: 86%

Setting the Stage for Planet Formation: Measurements and Implications of the Fundamental Disk Properties

Miotello¹,

Kamp²,

Birnstiel³

et al. 2022

Preprint

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The field of planet formation is in an exciting era, where recent observations of disks around low-to intermediate-mass stars made with state of the art interferometers and high-contrast optical and IR facilities have revealed a diversity of substructures, some possibly planet-related. It is therefore important to understand the physical and chemical nature of the protoplanetary building blocks, as well as their spatial distribution, to better understand planet formation. Since PPVI, the field has seen tremendous improvements in observational capabilities, enabling both surveys of large samples of disks and high resolution imaging studies of a few bright disks. Improvements in data quality and sample size have, however, opened up many fundamental questions about properties such as the mass budget of disks, its spatial distribution, and its radial extent. Moreover, the vertical structure of disks has been studied in greater detail with spatially resolved observations, providing new insights on vertical layering and temperature stratification, yet also bringing rise to questions about other properties, such as material transport and viscosity. Each one of these properties -disk mass, surface density distribution, outer radius, vertical extent, temperature structure, and transport -is of fundamental interest as they collectively set the stage for disk evolution and corresponding planet formation theories. In this chapter, we will review our understanding of the fundamental properties of disks including the relevant observational techniques to probe their nature, modeling methods, and the respective caveats. Finally, we discuss the implications for theories of disk evolution and planet formation underlining what new questions have since arisen as our observational facilities have improved. Recent observational results, combined with advances in disk physical and chemical modelling, have resulted in a much more detailed and complex picture of the planet form-Protostars and Planets VII

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Section: Gas Mass From Hd Emission -supporting

confidence: 86%

Setting the Stage for Planet Formation: Measurements and Implications of the Fundamental Disk Properties

Miotello¹,

Kamp²,

Birnstiel³

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

“…This could be the case if the material originated from within the protoplanetary disks because the gas-to-dust and 12 CO:H 2 ratios in disks are both expected to decrease over time (e.g., Gorti et al 2015;Miotello et al 2019). Sturm et al (2022) find evidence from [C I] observations that carbon is depleted by a factor of 17 from ISM levels in the outer regions of the DO Tau disk, which would in turn reduce the 12 CO:H 2 ratio. Wide-field observations with better uv coverage will be necessary to robustly examine the consistency between the 13 CO-derived mass and the Herschel-derived mass.…”

Section: Mass Constraints On Structures Surrounding Do Taumentioning

confidence: 99%

“…It will also be useful to improve constraints on DO Tau's C/O ratio, which is expected to increase between the Class I and II stages (e.g., Cleeves et al 2018;Miotello et al 2019). Results have thus far been mixed; Sturm et al (2022) derived a relatively high C/O ratio of ∼1 based on spatially unresolved [C I] observations but found that the C 2 H upper limit from Bergner et al (2019) was better explained by an ISM-like ratio of 0.47. Obtaining deeper and higher resolutions of [C I] and C 2 H, or estimating the C/O ratio from SO/CS, can help to resolve this ambiguity.…”

Section: Avenues For Clarifying the Origins Of Do Tau's Extended Stru...mentioning

confidence: 99%

Disk Evolution Study through Imaging of Nearby Young Stars (DESTINYS): A Panchromatic View of DO Tau’s Complex Kilo-astronomical-unit Environment

Huang

Ginski

Benisty

et al. 2022

ApJ

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While protoplanetary disks are often treated as isolated systems in planet formation models, observations increasingly suggest that vigorous interactions between Class II disks and their environments are not rare. DO Tau is a T Tauri star that has previously been hypothesized to have undergone a close encounter with the HV Tau system. As part of the DESTINYS ESO Large Programme, we present new Very Large Telescope (VLT)/SPHERE polarimetric observations of DO Tau and combine them with archival Hubble Space Telescope (HST) scattered-light images and Atacama Large Millimeter/submillimeter Array (ALMA) observations of CO isotopologues and CS to map a network of complex structures. The SPHERE and ALMA observations show that the circumstellar disk is connected to arms extending out to several hundred astronomical units. HST and ALMA also reveal stream-like structures northeast of DO Tau, some of which are at least several thousand astronomical units long. These streams appear not to be gravitationally bound to DO Tau, and comparisons with previous Herschel far-IR observations suggest that the streams are part of a bridge-like structure connecting DO Tau and HV Tau. We also detect a fainter redshifted counterpart to a previously known blueshifted CO outflow. While some of DO Tau’s complex structures could be attributed to a recent disk–disk encounter, they might be explained alternatively by interactions with remnant material from the star formation process. These panchromatic observations of DO Tau highlight the need to contextualize the evolution of Class II disks by examining processes occurring over a wide range of size scales.

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“…This could be the case if the material originated from within the protoplanetary disks, since the gas-to-dust and 12 CO:H 2 ratios in disks are both expected to decrease over time (e.g., Gorti et al 2015;Miotello et al 2019). Sturm et al (2022) find evidence from [C I] observations that carbon is depleted by a factor of 17 from ISM levels in the outer regions of the DO Tau disk, which would in turn reduce the 12 CO:H 2 ratio. Widefield observations with better uv coverage will be necessary to robustly examine the consistency between the 13 CO-derived mass and the Herschel-derived mass.…”

Section: Mass Constraints On Structures Surrounding Do Taumentioning

confidence: 99%

“…It will also be useful to improve constraints on DO Tau's C/O ratio, which is expected to decrease between the Class I and II stages (e.g., Cleeves et al 2018;Miotello et al 2019). Results have thus far been mixed; Sturm et al (2022) derived a relatively high C/O ratio of ∼ 1 based on spatially unresolved [C I]] obervations but found that the C 2 H upper limit from Bergner et al (2019) was better explained by an ISM-like ratio of 0.47. Obtaining deeper and higher resolutions of [C I] and C 2 H, or estimating the C/O ratio from SO/CS, can help to resolve this ambiguity.…”

Section: Evidence For Remnant Envelope Materialsmentioning

confidence: 99%

Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): A Panchromatic View of DO Tau's Complex Kilo-au Environment

Huang,

Ginski,

Benisty

et al. 2022

Preprint

View full text Add to dashboard Cite

While protoplanetary disks are often treated as isolated systems in planet formation models, observations increasingly suggest that vigorous interactions between Class II disks and their environments are not rare. DO Tau is a T Tauri star that has previously been hypothesized to have undergone a close encounter with the HV Tau system. As part of the DESTINYS ESO Large Programme, we present new VLT/SPHERE polarimetric observations of DO Tau and combine them with archival HST scattered light images and ALMA observations of CO isotopologues and CS to map a network of complex structures. The SPHERE and ALMA observations show that the circumstellar disk is connected to arms extending out to several hundred au. HST and ALMA also reveal stream-like structures northeast of DO Tau, some of which are at least several thousand au long. These streams appear not to be gravitationally bound to DO Tau, and comparisons with previous Herschel far-IR observations suggest that the streams are part of a bridge-like structure connecting DO Tau and HV Tau. We also detect a fainter redshifted counterpart to a previously known blueshifted CO outflow. While some of DO Tau's complex structures could be attributed to a recent disk-disk encounter, they might be explained alternatively by interactions with remnant material from the star formation process. These

show abstract

Tracing pebble drift and trapping using radial carbon depletion profiles in protoplanetary disks

Cited by 4 publications

References 84 publications

Setting the Stage for Planet Formation: Measurements and Implications of the Fundamental Disk Properties

Setting the Stage for Planet Formation: Measurements and Implications of the Fundamental Disk Properties

Disk Evolution Study through Imaging of Nearby Young Stars (DESTINYS): A Panchromatic View of DO Tau’s Complex Kilo-astronomical-unit Environment

Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): A Panchromatic View of DO Tau's Complex Kilo-au Environment

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