Kinematic Structures in Planet-Forming Disks

Pinte, C.; Flaherty, Kevin R.; Hall, Cassandra; Facchini, Stefano; Casassus, S.

doi:10.48550/arxiv.2203.09528

Cited by 37 publications

(47 citation statements)

References 302 publications

(416 reference statements)

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“…Although this task has long been challenging, the situation is rapidly changing. In particular, recent observations with the Atacama Large Millimeter/submillimeter Array (ALMA) have demonstrated the possibility of detecting young planets by spatially and kinematically resolving the characteristic gas flows around forming planets (see review by Pinte et al 2022), including localized velocity perturbations associated with planet-driven spirals (Pinte et al 2018;) and large-scale meridional flows falling on to planet-hosting gaps (Teague et al 2019a;Yu et al 2021).…”

Section: Introductionmentioning

confidence: 99%

Molecules with ALMA at Planet-forming Scales (MAPS): A Circumplanetary Disk Candidate in Molecular-line Emission in the AS 209 Disk

Bae

Andrews

Benisty

et al. 2022

ApJL

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We report the discovery of a circumplanetary disk (CPD) candidate embedded in the circumstellar disk of the T Tauri star AS 209 at a radial distance of about 200 au (on-sky separation of 1.″4 from the star at a position angle of 161°), isolated via 13CO J = 2−1 emission. This is the first instance of CPD detection via gaseous emission capable of tracing the overall CPD mass. The CPD is spatially unresolved with a 117 × 82 mas beam and manifests as a point source in 13CO, indicating that its diameter is ≲14 au. The CPD is embedded within an annular gap in the circumstellar disk previously identified using 12CO and near-infrared scattered-light observations and is associated with localized velocity perturbations in 12CO. The coincidence of these features suggests that they have a common origin: an embedded giant planet. We use the 13CO intensity to constrain the CPD gas temperature and mass. We find that the CPD temperature is ≳35 K, higher than the circumstellar disk temperature at the radial location of the CPD, 22 K, suggesting that heating sources localized to the CPD must be present. The CPD gas mass is ≳0.095 M Jup ≃ 30 M ⊕ adopting a standard 13CO abundance. From the nondetection of millimeter continuum emission at the location of the CPD (3σ flux density ≲26.4 μJy), we infer that the CPD dust mass is ≲0.027 M ⊕ ≃ 2.2 lunar masses, indicating a low dust-to-gas mass ratio of ≲9 × 10−4. We discuss the formation mechanism of the CPD-hosting giant planet on a wide orbit in the framework of gravitational instability and pebble accretion.

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Section: Introductionmentioning

confidence: 99%

Molecules with ALMA at Planet-forming Scales (MAPS): A Circumplanetary Disk Candidate in Molecular-line Emission in the AS 209 Disk

Bae

Andrews

Benisty

et al. 2022

ApJL

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“…Given the challenges of directly detecting young planet photospheres, efforts from various indirect avenues are essential to confirm the planet origin of disk substructures. One recent advance is the detection of localized velocity deviations from Keplerian motion in the gas disk, where the perturbation amplitude is linked to the planet mass (Pinte et al 2022). Another option aims to probe disk material that feeds the growth of a planet through a circumplanetary disk (CPD), on scales smaller than the Hill radius.…”

Section: Introductionmentioning

confidence: 99%

ALMA Detection of Dust Trapping around Lagrangian Points in the LkCa 15 Disk

Long

Andrews

Zhang

et al. 2022

ApJL

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We present deep high-resolution (∼50 mas, 8 au) Atacama Large Millimeter/submillimeter Array (ALMA) 0.88 and 1.3 mm continuum observations of the LkCa 15 disk. The emission morphology shows an inner cavity and three dust rings at both wavelengths, but with slightly narrower rings at the longer wavelength. Along a faint ring at 42 au, we identify two excess emission features at ∼10σ significance at both wavelengths: one as an unresolved clump and the other as an extended arc, separated by roughly 120° in azimuth. The clump is unlikely to be a circumplanetary disk (CPD) as the emission peak shifts between the two wavelengths even after accounting for orbital motion. Instead, the morphology of the 42 au ring strongly resembles the characteristic horseshoe orbit produced in planet–disk interaction models, where the clump and the arc trace dust accumulation around Lagrangian points L 4 and L 5, respectively. The shape of the 42 au ring, dust trapping in the outer adjacent ring, and the coincidence of the horseshoe ring location with a gap in near-IR scattered light, are all consistent with the scenario of planet sculpting, with the planet likely having a mass between those of Neptune and Saturn. We do not detect pointlike emission associated with a CPD around the putative planet location (0.″27 in projected separation from the central star at a position angle of ∼60°), with upper limits of 70 and 33 μJy at 0.88 and 1.3 mm, respectively, corresponding to dust mass upper limits of 0.02–0.03 M ⊕.

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“…Theoretical studies show that when the disk turbulence is high, dust trapping in pressure maxima is far less efficient than in the case of low turbulent amplitudes (Pinilla et al 2020). The most recent compilation of a wide range of data and methods finds that typically α turb ∼ 10 −3 − 10 −4 (Pinte et al 2022). This extensive set of observations suggests that a range of turbulent viscosities is intrinsic to protoplanetary disk populations and we incorporate this into the evolution of our planetary populations.…”

Section: Introductionmentioning

confidence: 97%

Combined effects of disc winds and turbulence-driven accretion on planet populations

Alessi

2022

Monthly Notices of the Royal Astronomical Society

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Recent surveys show that protoplanetary disks have lower levels of turbulence than expected based on their observed accretion rates. A viable solution to this is that magnetized disk winds dominate angular momentum transport. This has several important implications for planet formation processes. We compute the physical and chemical evolution of disks and the formation and migration of planets under the combined effects of angular momentum transport by turbulent viscosity and disk winds. We take into account the critical role of planet traps to limit Type I migration in all of these models and compute thousands of planet evolution tracks for single planets drawn from a distribution of initial disk properties and turbulence strengths. We do not consider multi-planet models nor include N-body planet-planet interactions. Within this physical framework we find that populations with a constant value disk turbulence and winds strength produce mass-semimajor axis distributions in the M-a diagram with insufficient scatter to compare reasonably with observations. However, populations produced as a consequence of sampling disks with a distribution of the relative strengths of disk turbulence and winds fit much better. Such models give rise to a substantial super Earth population at orbital radii 0.03-2 AU, as well as a clear separation between the produced hot Jupiter and warm Jupiter populations. Additionally, this model results in a good comparison with the exoplanetary mass-radius distribution in the M-R diagram after post-disk atmospheric photoevaporation is accounted for.

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Kinematic Structures in Planet-Forming Disks

Cited by 37 publications

References 302 publications

Molecules with ALMA at Planet-forming Scales (MAPS): A Circumplanetary Disk Candidate in Molecular-line Emission in the AS 209 Disk

Molecules with ALMA at Planet-forming Scales (MAPS): A Circumplanetary Disk Candidate in Molecular-line Emission in the AS 209 Disk

ALMA Detection of Dust Trapping around Lagrangian Points in the LkCa 15 Disk

Combined effects of disc winds and turbulence-driven accretion on planet populations

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