High gas-to-dust size ratio indicating efficient radial drift in the mm-faint CX Tauri disk

Facchini, Stefano; Dishoeck, E. van; Manara, C. F.; Tazzari, Marco; Maud, L. T.; Cazzoletti, P.; Rosotti, Giovanni; Marel, Nienke van der; Pinilla, P.; Clarke, C. J.

doi:10.1051/0004-6361/201935496

Cited by 68 publications

(62 citation statements)

References 54 publications

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“…We find that four of our six disks show a ratio between the R 90,gas and R 90,dust that is very close to or above 4.0, which is similar to the ratio measured in CX Tau (Facchini et al 2019) (ratio of 3.9 ± 0.5 at R 90 ), as compared in Fig. 7.…”

Section: R Gas /R Dust Ratiosupporting

confidence: 86%

“…A more complete sample, which includes more observations of disks around very low and moderate mass stars, and also uniform data sensitivity and analysis are required to confirm if there is a general trend where R gas /R dust increases towards lower stellar masses. (2018) (abbreviated as A+18), CX Tau (Facchini et al 2019), and the targets reported in this paper. For CX Tau, we took the R 90 radii of the dust and gas.…”

Section: R Gas /R Dust Ratiomentioning

confidence: 99%

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Size and structures of disks around very low mass stars in the Taurus star-forming region

Kurtovic

Pinilla

Long

et al. 2021

A&A

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Context. The discovery of giant planets orbiting very low mass stars (VLMS) and the recent observed substructures in disks around VLMS is challenging planet formation models. Specifically, radial drift of dust particles is a catastrophic barrier in these disks, which prevents the formation of planetesimals and therefore planets. Aims. We aim to estimate if structures, such as cavities, rings, and gaps, are common in disks around VLMS and to test models of structure formation in these disks. We also aim to compare the radial extent of the gas and dust emission in disks around VLMS, which can give us insight about radial drift. Methods. We studied six disks around VLMS in the Taurus star-forming region using ALMA Band 7 (~340 GHz) at a resolution of ~0.1″. The targets were selected because of their high disk dust content in their stellar mass regime. Results. Our observations resolve the disk dust continuum in all disks. In addition, we detect the 12CO (J = 3−2) emission line in all targets and 13CO (J = 3−2) in five of the six sources. The angular resolution allows the detection of dust substructures in three out of the six disks, which we studied by using UV-modeling. Central cavities are observed in the disks around stars MHO 6 (M 5.0) and CIDA 1 (M 4.5), while we have a tentative detection of a multi-ringed disk around J0433. We estimate that a planet mass of ~0.1 MJup or ~0.4 MSaturn is required for a single planet to create the first gap in J0433. For the cavities of MHO 6 and CIDA 1, a Saturn-mass planet (~0.3 MJup) is required. The other three disks with no observed structures are the most compact and faintest in our sample, with the radius enclosing 90% of the continuum emission varying between ~13 and 21 au. The emission of 12CO and 13CO is more extended than the dust continuum emission in all disks of our sample. When using the 12CO emission to determine the gas disk extension Rgas, the ratio of Rgas∕Rdust in our sample varies from 2.3 to 6.0. One of the disks in our sample, CIDA 7, has the largest Rgas∕Rdust ratio observed so far, which is consistent with models of radial drift being very efficient around VLMS in the absence of substructures. Conclusions. Given our limited angular resolution, substructures were only directly detected in the most extended disks, which represent 50% of our sample, and there are hints of unresolved structured emission in one of the bright smooth sources. Our observations do not exclude giant planet formation on the substructures observed. A comparison of the size and luminosity of VLMS disks with their counterparts around higher mass stars shows that they follow a similar relation.

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Section: R Gas /R Dust Ratiosupporting

confidence: 86%

Section: R Gas /R Dust Ratiomentioning

confidence: 99%

Size and structures of disks around very low mass stars in the Taurus star-forming region

Kurtovic

Pinilla

Long

et al. 2021

A&A

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“…From both Kudo et al 2018;Huélamo et al 2015) this difference is still quite large for UX Tauri A. However, Facchini et al (2019) reported in CX Tauri a large difference of the millimeter dust and gas extents (> 5) and argue that the this could be explained due to a radial drift, and closely matches the predictions of theoretical models. This difference in dust and gas extents is notorious for UX Tauri A, however, it is not clear for UX Tau C because we did not detect the continuum emission.…”

Section: Ux Tauri System (A/c)supporting

confidence: 73%

Tidal Interaction between the UX Tauri A/C Disk System Revealed by ALMA

Zapata¹,

Rodrı́guez

Fernández-López

et al. 2020

ApJ

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We present sensitive and high angular resolution (∼0.2-0.3 ) (sub)millimeter (230 and 345 GHz) continuum and CO(2−1)/CO(3−2) line archive observations of the disk star system in UX Tauri carried out with ALMA (The Atacama Large Millimeter/Submillimeter Array). These observations reveal the gas and dusty disk surrounding the young star UX Tauri A with a large signal-to-noise ratio (>400 in the continuum and >50 in the line), and for the first time is detected the molecular gas emission associated with the disk of UX Tauri C (with a size for the disk of <56 au). No (sub)millimeter continuum emission is detected at 5σ-level (0.2 mJy at 0.85 mm) associated with UX Tauri C. For the component UX Tauri C, we estimate a dust disk mass of ≤ 0.05 M ⊕ . Additionally, we report a strong tidal disk interaction between both disks UX Tauri A/C, separated 360 au in projected distance. The CO line observations reveal marked spiral arms in the disk of UX Tauri A and an extended redshifted stream of gas associated with the UX Tauri C disk. No spiral arms are observed in the dust continuum emission of UX Tauri A. Assuming a Keplerian rotation we estimate the enclosed masses (disk+star) from their radial velocities in 1.4 ± 0.6 M for UX Tauri A, and 70 ± 30 / sin i Jupiter masses for UX Tauri C (the latter coincides with the mass upper limit value for a brown dwarf). The observational evidence presented here lead us to propose that UX Tauri C is having a close approach of a possible wide, evolving and eccentric orbit around the disk of UX Tauri A causing the formation of spiral arms and the stream of molecular gas falling towards UX Tauri C.

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“…This is a conservative choice in terms of the observed range of values (Isella et al 2016;Ansdell et al 2018;Facchini et al 2019) that mimics the HD 163296ʼs radial behavior of gas and dust. The solids concentration factor ξ is used in conjunction with the mass fraction of condensed material Z i (shown in Figure 2 and described in Section 2.5 and Table 3) to compute the radial distribution of solids…”

Section: Planetesimal Disk and Time Step Of The Simulationsmentioning

confidence: 99%

Tracing the Formation History of Giant Planets in Protoplanetary Disks with Carbon, Oxygen, Nitrogen, and Sulfur

Turrini

Schisano

Fonte

et al. 2021

ApJ

129

229

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The composition of giant planets is imprinted by their migration history and the compositional structure of their hosting disks. Studies in recent literature have investigated how the abundances of C and O can constrain the formation pathways of giant planets forming within few tens of au from a star. New ALMA observations, however, suggest planet-forming regions possibly extending to hundreds of au. We explore the implications of these wider formation environments through n-body simulations of growing and migrating giant planets embedded in planetesimal disks, coupled with a compositional model of the protoplanetary disk where volatiles are inherited from the molecular cloud and refractories are calibrated against extrasolar and Solar System data. We find that the C/O ratio provides limited insight on the formation pathways of giant planets that undergo large-scale migration. This limitation can be overcome, however, thanks to nitrogen and sulfur. Jointly using the C/N, N/O, and C/O ratios breaks any degeneracy in the formation and migration tracks of giant planets. The use of elemental ratios normalized to the respective stellar ratios supplies additional information on the nature of giant planets, thanks to the relative volatility of O, C, and N in disks. When the planetary metallicity is dominated by the accretion of solids C/N * > C/O * > N/O * ( * denoting this normalized scale), otherwise N/O * > C/O * > C/N * . The S/N ratio provides an additional independent probe into the metallicity of giant planets and their accretion of solids.

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High gas-to-dust size ratio indicating efficient radial drift in the mm-faint CX Tauri disk

Cited by 68 publications

References 54 publications

Size and structures of disks around very low mass stars in the Taurus star-forming region

Size and structures of disks around very low mass stars in the Taurus star-forming region

Tidal Interaction between the UX Tauri A/C Disk System Revealed by ALMA

Tracing the Formation History of Giant Planets in Protoplanetary Disks with Carbon, Oxygen, Nitrogen, and Sulfur

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