Gap Opening and Inner Disk Structure in the Strongly Accreting Transition Disk of DM Tau

Francis, Logan; Marel, Nienke van der; Johnstone, Doug; Akiyama, Eiji; Bruderer, S.; Dong, Ruobing; Hashimoto, Jun; Liu, Hauyu Baobab; Muto, Takayuki; Yang, Yi

doi:10.3847/1538-3881/ac7ffb

Cited by 7 publications

(6 citation statements)

References 78 publications

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“…The measured accretion rates for the 13 disks with inverse P Cygni-like Lyα emission range from M M 5 10 3 10 ´-  yr −1 for CVSO 109A; Pittman et al 2022), confirming that accretion rates can remain high even as material is dissipated from the outer disks. This is consistent with submm observations, which still show significant gas abundances in disks with high accretion rates and large dust cavities or gaps (see, e.g., Bruderer 2013;Espaillat et al 2014;Kudo et al 2018;Francis et al 2022).…”

Section: Model H I Velocities Probe Kinematics Of Accretion and Outflowssupporting

confidence: 89%

“…DM Tau shows opposite behavior, where infalling H I has absorbed photons on the red side of the line profile. The schematic on the right illustrates this stage, showing that large dust gaps consistent with models of planet-disk interactions have been cleared in the dust distributions (see, e.g., DM Tau; Hashimoto et al 2021;Francis et al 2022). Low-velocity components of [O I] 6300 Å and [Ne II] 12.81 μm emission lines are still observed, consistent with origins in MHD winds (see, e.g., Banzatti et al 2019;Pascucci et al 2020) or photoevaporative flows (Pascucci & Sterzik 2009).…”

Section: Shell Models With Lyα Emission and Absorptionmentioning

confidence: 64%

“…Residual optically thick, gas-rich inner disks may linger, however, as evidenced by large accretion rates derived from Hα emission, U band excess (Najita et al 2007;Espaillat et al 2012), and UV-near-infrared continuum fits (Manara et al 2014) for many transitional disk systems with disk dust gaps or cavities that may be associated with protoplanet formation. Such reservoirs have subsequently been resolved around TW Hya (Ercolano & Pascucci 2017), SR 24S and CIDA 1 (Pinilla et al 2019(Pinilla et al , 2021, DM Tau (Hashimoto et al 2021;Francis et al 2022), and LkCa 15 (Blakely et al 2022).…”

Section: Introductionmentioning

confidence: 99%

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Lyα Scattering Models Trace Accretion and Outflow Kinematics in T Tauri Systems*

Arulanantham

Grönke

Fiorellino

et al. 2023

ApJ

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T Tauri stars produce broad Lyα emission lines that contribute ∼88% of the total UV flux incident on the inner circumstellar disks. Lyα photons are generated at the accretion shocks and in the protostellar chromospheres and must travel through accretion flows, winds, and jets, the protoplanetary disks, and the interstellar medium before reaching the observer. This trajectory produces asymmetric, double-peaked features that carry kinematic and opacity signatures of the disk environments. To understand the link between the evolution of Lyα emission lines and the disks themselves, we model HST-COS spectra from targets included in Data Release 3 of the Hubble UV Legacy Library of Young Stars as Essential Standards program. We find that resonant scattering in a simple spherical expanding shell is able to reproduce the high-velocity emission line wings, providing estimates of the average velocities within the bulk intervening H i. The model velocities are significantly correlated with the K-band veiling, indicating a turnover from Lyα profiles absorbed by outflowing winds to emission lines suppressed by accretion flows as the hot inner disk is depleted. Just 30% of targets in our sample have profiles with redshifted absorption from accretion flows, many of which have resolved dust gaps. At this stage, Lyα photons may no longer intersect with disk winds along the path to the observer. Our results point to a significant evolution of Lyα irradiation within the gas disks over time, which may lead to chemical differences that are observable with ALMA and JWST.

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Section: Model H I Velocities Probe Kinematics Of Accretion and Outflowssupporting

confidence: 89%

Section: Shell Models With Lyα Emission and Absorptionmentioning

confidence: 64%

Section: Introductionmentioning

confidence: 99%

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Lyα Scattering Models Trace Accretion and Outflow Kinematics in T Tauri Systems*

Arulanantham

Grönke

Fiorellino

et al. 2023

ApJ

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“…However, if the high accretion rate implied by observations is generated by magnetorotational instability viscosity, it would mean that this source is not a low-viscosity but a high-viscosity system (Delage et al 2022). This would require a sufficiently massive planet (maybe nearly 10 times the mass of Jupiter) to produce such structures (Pinilla et al 2012;Francis et al 2022). Moreover, massive planets will carve out eccentric gaps and generate streamer structures (Chen et al 2024); thus, the hypothesis of a single massive planet would have difficulty generating the observed asymmetric structures in DM Tau.…”

Section: The Dm Tau Disk Systemmentioning

confidence: 99%

Asymmetry, Gap Opening, and a High Accretion Rate on DM Tau: A Hypothesis Based on the Interaction of Magnetized Disk Wind with Planets

Wu 吴

2024

ApJ

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Over 200 protoplanetary disk systems have been resolved by the Atacama Large Millimeter/submillimeter Array (ALMA), and the vast majority suggest the presence of planets. The dust gaps in transition disks are considered evidence of giant planets sculpting gas and dust under appropriate disk viscosity. However, the unusually high accretion rates in many T Tauri stars hosting transition disks challenge this theory. As the only disk currently observed with high turbulence, the high accretion rate (∼10−8.3 M ⊙ yr−1) observed in DM Tau indicates the presence of strong turbulence within the system. Considering the recent theoretical advancements in magnetized disk winds are challenging the traditional gap-opening theories and viscosity-driven accretion models, our study presents a pioneering simulation incorporating a simplified magnetized disk wind model to explain the observed features in DM Tau. Employing multifluid simulations with an embedded medium mass planet, we successfully replicate the gap formation and asymmetric structures evident in ALMA Band 6 and the recent Karl G. Jansky Very Large Array 7 mm observations. Our results suggest that when magnetized disk wind dominates the accretion mode of the system, it is entirely possible for a planet with a medium mass to exist within the gap inside 20 au of DM Tau. This means that DM Tau may not be as turbulent as imagined. However, viscosity within the disk should also contribute a little turbulence to maintain disk stability.

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“…For disks in which only upper limits were obtained with HIFI and PACS, only DM Tau (for which deep observations have been obtained at 269.27 and 538.29 μm) is notably discrepant with the models. While we do not have a model specific to this disk, Francis et al (2022) recently modeled spatially resolved ALMA emission from the DM Tau disk in detail and derived gas and dust masses of ∼6 × 10 −3 and ∼6 × 10 −4 M e , respectively. Their adopted surface density distribution is very similar to our models for the same mass disk, and tapers off at r = 126 au.…”

Section: Comparison With Observationsmentioning

confidence: 99%

Cold Water Emission Cannot Be Used to Infer Depletion of Bulk Elemental Oxygen [O/H] in Disks

Ruaud,

Gorti

2024

ApJ

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We reexamine the constraints provided by Herschel Space Observatory data regarding cold water emission from protoplanetary disks. Previous disk models that were used to interpret observed water emission concluded that oxygen (O/H) is depleted by at least 2 orders of magnitude if a standard, interstellar gas/dust mass ratio is assumed in the disk. In this work, we use model results from a recent disk parameter survey and show that most of the Herschel constraints obtained for cold water (i.e., for transitions with an upper energy level E up < 200 K, where the bulk of the disk water lies) can be explained with disk models adopting interstellar medium-like oxygen elemental abundance (i.e., O/H = 3.2 × 10−4) and the canonical gas/dust mass ratio of 100. We show that cold water vapor is mainly formed by photodesorption of water ice at the interface between the molecular layer and the midplane, and that its emission is relatively independent of the main disk properties like the disk gas mass and gas/dust mass ratio. We find that the abundance of water vapor in the outer disk is set by photoprocesses and depends on the (constant) vertical column density of water ice needed to attenuate the far-ultraviolet photon flux, resulting in roughly constant emission for the parameters (gas mass, dust mass, disk radius) varied in our survey. Importantly, water line emission is found to be optically thick and hence sensitive to temperature more than abundance, possibly driving previous inferences of large-scale oxygen depletion.

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Gap Opening and Inner Disk Structure in the Strongly Accreting Transition Disk of DM Tau

Cited by 7 publications

References 78 publications

Lyα Scattering Models Trace Accretion and Outflow Kinematics in T Tauri Systems*

Lyα Scattering Models Trace Accretion and Outflow Kinematics in T Tauri Systems*

Asymmetry, Gap Opening, and a High Accretion Rate on DM Tau: A Hypothesis Based on the Interaction of Magnetized Disk Wind with Planets

Cold Water Emission Cannot Be Used to Infer Depletion of Bulk Elemental Oxygen [O/H] in Disks

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