Dust transport in envelopes of disk-embedded planets: II. Fully convective envelopes

Ayumu Kuwahara; Michiel Lambrechts

REVIEW 3 major objections 5 minor 300 references

Dust transport in envelopes of disk-embedded planets: II. Fully convective envelopes

T0 review · 3 major / 5 minor · reviewed 2026-08-08 · deepseek-v4-flash

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Pith's one-line read Whether a forming planet's envelope keeps dust comes down to one thing: is it open to the disk or sealed off by a recycling flow?

desk verdict Solid sequel to KL26b with a genuinely new dust-retention dichotomy, but the central regime split currently rests on a hand-set one-cell cooling step at the Bondi radius. read the letter →

arxiv 2608.05672 v1 pith:5CX2BTFC submitted 2026-08-06 astro-ph.EP

Ayumu Kuwahara , Michiel Lambrechts This is my paper · ORCID

classification astro-ph.EP

keywords dusttransportplanetaryenvelopesconvectionprotoplanetarydiskspebbleaccretiondust-to-gasratioplanetformation

verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

This paper asks whether the convective envelopes of disk-embedded planets retain the dust they accrete or lose it. Using 3D multifluid simulations of gas and dust around an Earth-mass planet, the authors find that the dust-to-gas ratio inside the envelope is set primarily by how dynamically isolated the envelope is from the disk: if convection extends beyond the Bondi radius the envelope exchanges gas with the disk continuously and stays dust-rich, whereas if an inner convective layer is sealed off from an outer recycling layer, that recycling flow filters out incoming solids and the envelope becomes dust-depleted. Inside the isolated layer the fate of dust is decided by a race between convective stirring and gravitational settling, which traps grains smaller than roughly $s \lesssim 0.01$ cm and lets larger grains fall to the core. The paper's picture implies that where a planet forms decides what its envelope and core are made of, offering an explanation for the wide diversity of mini-Neptune atmospheric compositions.

What carries the argument

The argument is carried by a cooling-time prescription that dials the envelope between two end-member states: the dimensionless cooling time $\beta \equiv t_{\rm cool}\Omega$, with a constant value $\beta = 10^3$ giving a non-isolated, fully convective envelope, and a radially varying profile that steps from $\beta_{\min}=10^0$ outside to $\beta_{\max}=10^3$ inside the Bondi radius $R_B$, giving an isolated convective interior with a recycling flow outside. Accretion luminosity $L_{\rm acc}$ heats the deep envelope and sustains the convection. Within the envelope, the competition between the mixing-length convective velocity $v_{\rm con} \propto (l_m L_{\rm acc})^{1/3}$ and the terminal settling velocity $v_{\rm term}$ sets whether grains are trapped or settle, and a one-dimensional steady-flux model $\rho_d(r) = \dot{M}_{d,\rm acc}/(4\pi r^2 v_{d,\rm in}(r))$, with a collision rate modified by recycling outflow and convective inflow, reproduces the simulated dust-to-gas ratios.

What would settle it

Rerun the isolated-envelope configuration with a smooth cooling-time transition of width much larger than $0.01 R_B$, as the paper's own cooling-time estimate suggests, and check whether the dust-to-gas ratio still drops sharply at $r \simeq R_B$; if the depletion boundary smears or moves, the isolation dichotomy is an artifact of the step prescription. A second check is to vary the accretion luminosity $\tilde{L}_{\rm acc}$ and confirm that the trapping threshold shifts according to $v_{\rm con} \propto L_{\rm acc}^{1/3}$.

Watch

Extended reading notes

Core claim

The central claim is that convective envelopes come in two dynamical states with opposite consequences for dust. In the non-isolated state, realized when convection extends beyond the Bondi radius, the envelope is continuously flushed by the surrounding disk flow and the shell-averaged dust-to-gas ratio stays near $\epsilon \sim 10^{-3}$ to $10^{-2}$, because dust enters through a polar accretion pathway and is lofted by convection. In the isolated state, realized when the envelope is convective only inside the Bondi radius and a positive entropy gradient blocks inflow outside it, a recycling flow with polar inflow and midplane outflow filters incoming solids, and the dust-to-gas ratio drops by more than two orders of magnitude across $r \simeq R_B$. Within the isolated convective layer, dust retention is governed by whether the mixing-length convective velocity $v_{\rm con}$ exceeds the terminal settling velocity $v_{\rm term}$: small grains ($s \lesssim 0.01$ cm) are trapped in convective circulation and keep the envelope dusty, while larger grains ($s \gtrsim 0.1$ cm) settle at terminal velocity and deplete it. The authors extend their previous one-dimensional analytic model to this convective regime and reproduce the simulated dust-to-gas profiles.

Load-bearing premise

The load-bearing premise is that the two envelope states are produced by the prescribed cooling-time profile — a uniformly long cooling time that keeps convection alive beyond the Bondi radius versus a sharp step at the Bondi radius that seals the envelope off — even though the paper concedes that no single opacity model produces that structure and that realistic envelopes have a finite radiative layer rather than a sharp step.

Editorial extensions

If this is right

Non-isolated convective envelopes, expected inside roughly 1 au, stay dust-rich and inherit near-disk compositions, giving inner super-Earths and mini-Neptunes volatile-poor cores and volatile-rich envelopes.
Isolated envelopes, expected beyond roughly 1-10 au, deplete small grains; larger pebbles still reach the core and release volatiles at the sublimation front, so the deep envelope can be volatile-enriched while the observable outer envelope stays closer to disk composition.
Dust accretion rates differ by orders of magnitude between the two states: recycling outflow suppresses pebble accretion, while inward convective motions at the Bondi radius enhance it.
Dust retention raises envelope opacity and slows cooling, which can delay runaway gas accretion in the inner disk, while dust-depleted outer envelopes cool faster and may favor gas giant formation.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

If the sharp step in the cooling time at the Bondi radius were replaced by the broad radiative-convective transition that the paper's own cooling-time estimate predicts, the sharp drop in dust-to-gas ratio at $R_B$ would likely smear out; the predicted inner/outer disk compositional dichotomy may be a gradient rather than a clean boundary.
The simulations neglect fragmentation, yet the paper's collision-speed estimate for 1 cm grains (about 1-10 m/s) is near typical fragmentation thresholds; if grains fragment they shrink into the convection-trapped size range, which could re-dust an isolated envelope.
A testable extension is that the size threshold between trapping and settling should shift with accretion luminosity, since $v_{\rm con} \propto L_{\rm acc}^{1/3}$; varying $\tilde{L}_{\rm acc}$ in the same setup would map where the dust-depletion boundary sits.

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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Desk Editor's Note

read the letter

Kuwahara & Lambrechts II is a real extension of their first paper: adding accretion luminosity to 3D multifluid sims and showing that convective envelopes split into a non-isolated dust-retaining state and an isolated dust-depleting state, with small grains (≲0.01 cm) trapped by convection. The simulations are internally consistent, time-averaged, and convergence-tested in App. C. That is genuine work and the regime picture is credible as an end-member mechanism.

The soft spot is exactly what the stress-test note says: the isolated/non-isolated dichotomy is generated by a step in the cooling β profile at r=RB with width w=0.01 RB, resolved by one grid cell. Appendix B concedes no single opacity model reproduces that step; realistic envelopes have a finite radiative layer. So the sharp depletion boundary at RB and the two-orders-of-magnitude drop are, at this point, properties of the imposed entropy barrier. The authors say this themselves in App. B, which is honest, but it does mean the central dichotomy is not yet demonstrated to be robust under self-consistent cooling.

The 1D analytic model is also partly fitted and partly imposed: ξ=0.08m is tuned to match the simulations, and Eq. 29's convection-dominated branch simply returns the initial ϵ0 whenever v_con > v_term. That branch isn't derived; it's a prescription. The settling-dominated branch does real work and reproduces the profiles, so the model is not empty, but its predictive content is lower than a reader might first think.

I do not think these soft spots are fatal. The paper is framed as idealized end-member sims and the limitation statements are right there. The right next step is radiative-transfer-coupled sims with dust-opacity feedback, which the authors flag. For a mechanism-guidance paper, the regime distinction likely survives qualitatively even if the sharp boundary moves.

Who is this for: anyone working on pebble accretion, envelope composition, or mini-Neptune atmospheric metallicity. It deserves a serious referee: the numerics are careful, the advance over KL26b and over Popovas et al. is real, and the limitations are stated rather than hidden. My recommendation: send to review, with the cooling prescription's influence on the main dichotomy as the central referee question.

Referee Report

3 major / 5 minor

Summary. This paper presents 3D multifluid (gas+dust) Athena++ simulations of an Earth-mass planet embedded in a protoplanetary disk, with thermal relaxation parameterized by a cooling time β and with accretion luminosity included. Two cooling prescriptions are compared: a constant β=10^3, which keeps the envelope convectively unstable beyond the Bondi radius, and a variable β profile that is a step from β=10^0 to β=10^3 at r=R_B with width 0.01 R_B. The authors find that the constant-β envelope remains dynamically connected to the disk and retains dust (ε≳10^-3), whereas the variable-β envelope is isolated by an outer recycling layer and becomes depleted by more than two orders of magnitude at R_B, except for small grains (s≲0.01 cm) that are trapped by convection. A 1D analytic model is extended to describe the settling-dominated and convection-dominated regimes, and the implications for the volatile content of super-Earths and mini-Neptunes are discussed.

Significance. If the results are robust, they are significant for planet formation: they identify dynamical isolation of the envelope as a controlling factor for dust retention and volatile delivery, and they connect envelope structure to the observed diversity of atmospheric metallicities. The numerical work is internally consistent and convergence-tested (Appendix C), the diagnostics are time-averaged over the last ten orbits, and the paper is unusually explicit about the idealized nature of its cooling treatment (Section 5.4 and Appendix B). However, the central regime dichotomy rests on a sharply imposed cooling-time discontinuity, and the analytic convection-dominated branch is assumed rather than derived, so the general claims require either additional robustness tests or a more cautious framing.

major comments (3)

[Sect. 2.4, Eq. (18); Appendix B; Fig. 4] The central distinction between non-isolated and isolated envelopes is produced by a step-function cooling-time profile whose transition width w=0.01 R_B is resolved by a single grid cell and therefore acts as a discontinuity at the Bondi radius. Appendix B explicitly concedes that no single opacity model reproduces both the envelope structure and the adopted cooling prescription, and that realistic envelopes contain a finite radiative layer separating the inner convective region from the outer recycling flow. Because the two-order-of-magnitude drop in ε at r≈R_B (Fig. 4) is the main evidence for the 'dynamical isolation' scenario, the authors should test the sensitivity of the depletion boundary and of the retention/depletion dichotomy to the transition width and location (e.g., w=0.1 and 0.5 R_B, or a smooth radiative-convective structure). Without such a test, the central claim that the dust-to-gas ratio is set primarily by the degree of dynamical isolation is not yet established beyond this specific prescription.
[Sect. 4, Eq. (29)] The analytic model's convection-dominated branch sets ε(r)=ε_0 whenever v_con>v_term for all r≤R_B. This is not derived from the dust continuity equation or from a mixing model; it simply returns the initial dust-to-gas ratio. The agreement with the simulations in Figs. 4 and 9b is therefore not an independent prediction but a restatement of the assumption that the dust is perfectly retained. The authors should either derive this branch from a steady-state dust balance (e.g., zero net radial flux or a diffusion–settling equilibrium) or explicitly present it as an empirical closure and test it against simulations with different initial ε_0. As written, the statement that the 'simulated dust-to-gas profiles agree well' (Sect. 4) is misleading for the convection-dominated regime.
[Sects. 2.4 and 3.3.2] The claimed threshold between settling-dominated and convection-dominated regimes (s≲0.01 cm versus s≳0.1 cm) is based on a single planet mass (m=0.1), a single accretion luminosity (t_acc=10^5 yr), and, for the fixed-size runs, a single orbital location (1 au). The authors note that v_con scales as (ℓ_m L_acc)^{1/3} (Eq. 24), so the threshold should shift with luminosity, but no parameter sweep is presented. The abstract and conclusions present the 0.01–0.1 cm boundary as a general result; it should be framed as a fiducial-value estimate, or the authors should vary L_acc and m to map the regime boundary.

minor comments (5)

[Sect. 2.2, Eq. (11)] The expression for Q_heat is not typeset clearly in Eq. (11); please verify the prefactor and dimensions, since the printed form is ambiguous.
[Introduction] The text contains a typo: 'mini-Netpunes' should be 'mini-Neptunes'.
[Conclusions] In the concluding paragraph, 's≲0.01,cm' contains an errant comma; it should read 's≲0.01 cm'.
[Sect. 3.2, Fig. 4] The 'dust-retaining' conclusion for the non-isolated case is based on the shell-averaged ε, while the midplane values are systematically lower (thin curves in Fig. 4). Since the discussion of observable atmospheric composition concerns the outer envelope, please also report density-weighted or midplane values and discuss whether the qualitative conclusion is affected.
[Appendix D, Eq. (D.8)] The parameter ξ=0.08m in the recycling-flow collision rate is chosen to 'better match our numerical results'; this makes the analytic model partly calibrated rather than fully predictive. Please state this more prominently in the main text when presenting the 1D model.

Circularity Check

2 steps flagged · score 6.0 of 10

The 3D regime findings are independent, but the 1D analytic model's convection-dominated branch is imposed (epsilon = epsilon0) and its recycling suppression parameter is fit to the simulations.

self definitional [Section 4, Eq. (29)]
"To account for dust retention by convection, we modeled the dust-to-gas ratio as ϵ(r)= { ϵ0, if convective and vcon(r)>vterm(r) ∀r≤RB, ρd(r)/ρg(r), otherwise. (29)"

The convection-dominated branch assigns ϵ=ϵ0, which is the initial dust-to-gas ratio prescribed in Sect. 2.3 ('with ϵ0=0.01 its initial value'). No dust-continuity or flux equation determines this value; dust retention is therefore imposed, not derived. When the paper says the dotted curves 'reproduce the numerical results,' it is checking an assumed branch, and the analytic 'prediction' in the convection-dominated regime is the model's own input. The independent content lives in the 3D simulations, not in this branch.
fitted input called prediction [Appendix D, Eqs. (D.8)-(D.10), used in Section 4]
"While Okamura & Kobayashi (2021) adopted ξ=0.1m, we use ξ=0.08m to better match our numerical results same as in KL26b."

The recycling-flow suppression of pebble accretion is controlled by ξ in u(RB)=−ξcs,0 (Eq. D.8), and that velocity enters Pcol,flow and Pcol,2D (Eq. D.10). Because ξ is explicitly calibrated to the same numerical runs whose dust-to-gas ratios the 1D model then claims to reproduce, the predicted filtering efficiency in isolated envelopes is partly fitted, not independently derived. The paper is transparent about the calibration, but this makes the 'prediction' in the settling-dominated branch of Eq. (29) depend on simulation output rather than first principles.

full rationale

The core 3D simulation results are not circular: the dust-to-gas contrast between constant-β and variable-β envelopes is measured from multifluid hydrodynamics, with resolution and inner-boundary convergence checks in Appendix C. The main limitation is robustness rather than circularity: the isolation dichotomy is produced by a prescribed cooling-time step at r=RB (Eq. 18, with a transition width resolved by one grid cell), and Appendix B concedes that 'no single opacity model reproduces the envelope structure and the adopted cooling prescription simultaneously' and that realistic envelopes would have a finite radiative layer. That concern weakens extrapolation to real envelopes but is not a reduction of the simulation outcome to its input. The circularity score of 6 comes specifically from the 1D analytic model: Eq. (29) sets the convection-dominated dust-to-gas ratio to the initial value ϵ0 by construction, and Appendix D calibrates the recycling suppression parameter ξ to the same numerical results that the model is said to predict. These are fitted or imposed elements inside the analytic model, so the model does not independently predict dust retention or filtering efficiency; the independent predictive content resides in the 3D simulations, for which the derivation chain is self-contained.

Assumptions & free parameters 4 free parameters · 5 assumptions · 0 invented entities

The central simulation results depend on prescribed cooling parameters (beta profile), a fixed luminosity, an initial dust scale height, and a collision-rate parameter tuned to the numerics. These are inputs, not outputs; the qualitative regime split is simulation-driven, but the quantitative 1D model is partly calibrated by construction.

free parameters (4)

beta cooling profile = constant beta0 = 10^3; variable beta_max = 10^3, beta_min = 10^0, r0 = RB, w = 0.01 RB
Prescribed by hand to create non-isolated and isolated end-member envelopes; not derived from radiative transfer (Sect. 2.4).
recycling-flow collision parameter xi = 0.08 m
Tuned to numerical results in Appendix D and KL26b; controls collision-rate suppression for isolated envelopes.
initial dust scale height H_d,0 = 0.1 H_g,0 = RB
Sets an initially dust-filled Bondi region, which matters for dust retention in isolated convection-dominated runs (Sect. 2.3).
accretion timescale t_acc = 10^5 yr (L_acc about 10^27 erg/s)
Prescribed luminosity that sustains convection; in reality luminosity couples to the evolving dust accretion rate (Sect. 2.2 and 5.4).

assumptions (5)

domain assumption Gas and dust are modeled as two fluids with drag coupling, with no dust back-reaction and no dust diffusion.
Invoked in Sect. 2.1, Eq. 1; valid for epsilon about 0.01 but would break at high dust concentrations reached in some enrichment scenarios.
ad hoc to paper Thermal relaxation is parameterized by a constant or step-function beta cooling time rather than radiative transfer.
Sect. 2.2 and Eq. 18; Appendix B states no single opacity model reproduces both the envelope structure and the adopted cooling step.
ad hoc to paper Convection is sustained by a fixed accretion luminosity, with no feedback of dust opacity or dust depletion on the luminosity.
Sect. 2.2 Eq. 11 and Sect. 5.4; sustainability of convection is acknowledged as uncertain.
domain assumption The shell-averaged dust flow can be represented by a 1D steady-state balance with radial inflow at v_d,in, with convective fluctuations canceling.
Sect. 3.3.1 and Eq. 27; the assumption breaks down for s less than about 0.01 cm, where the paper switches to the imposed Eq. 29 branch.
domain assumption For fixed-size runs, the planet is embedded in a passively irradiated disk at 1 au (Eq. 26).
Sect. 3.3.1; used to convert fixed Stokes numbers to physical grain sizes and collision-rate estimates.

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Cite this review

Pith. "Pith review of Dust transport in envelopes of disk-embedded planets: II. Fully convective envelopes." pith.science (2026). https://pith.science/paper/5CX2BTFC

@misc{pith2026260805672,
  author       = {Pith},
  title        = {Pith review of: Dust transport in envelopes of disk-embedded planets: II. Fully convective envelopes},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/5CX2BTFC}},
  note         = {Machine review of arXiv:2608.05672}
}

abstract

We perform 3D multifluid simulations of gas and dust to quantify how convection reshapes the spatial distribution of dust grains inside the envelopes of disk-embedded planets. Building on the first paper of this series, which explored convectively stable envelopes, we here consider envelopes in which convection is sustained by the accretion luminosity. The dust-to-gas ratio inside the planetary envelope is set primarily by the degree of dynamical isolation from the surrounding disk. When convection extends beyond the Bondi radius, the envelope remains connected to the disk flow and maintains a dust-rich state through continuous material exchange. Conversely, when an inner convective layer is separated from an outer recycling layer, the recycling flow filters incoming solids. The dust distribution inside the convective layer is then controlled by the competition between convective stirring and gravitational settling. This yields two regimes: a settling-dominated regime, in which large grains (typically $s\gtrsim0.1$ cm) fall at the terminal velocity and the envelope becomes dust depleted, and a convection-dominated regime, in which smaller grains are trapped in convective circulation and the envelope retains its dust. The delivery and release of volatile species from accreting solids at the envelope sublimation front, together with the efficiency of convective mixing, determine how this material is distributed between the core and envelope. Our findings imply that super-Earths and mini-Neptunes inside the water snowline have volatile-depleted cores and volatile-rich envelopes, while planets at wider orbits can have a wide diversity of envelope compositions from depleted to enriched. This compositional diversity for planetary envelopes appears to be consistent with the large diversity in observed atmospheric compositions of mini-Neptunes.

Figures

Figures reproduced from arXiv: 2608.05672 by the authors.

**Figure 1.** Shell-averaged density and temperature gradient for different β prescriptions, and cumulative volume-integrated heating and cooling rates. Top: Assumed hydrostatic equilibrium in adiabatic and isothermal limits is shown by the dotted and dashed curves(Eqs. 20 and 21). Middle: Adiabatic gradient (dotted line; Eq. 9). Bottom: Vertical axis normalized by the volume-integrated heating rate, R rout rin QheatdV. 3. Numer… view at source ↗

**Figure 2.** Density and velocity vector field of the gas averaged over the azimuth, ϕ ∈ [−π/2, π/2], for the two different β prescriptions at t = 93 (top) and t = 86 (bottom). The dashed white circle marks the Bondi radius. and for highlighting the differences from our previous study of convectively stable envelopes (KL26b) [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗

**Figure 5.** [PITH_FULL_IMAGE:figures/full_fig_p006_5.png] view at source ↗

Figures from the paper (6 more)

**Figure 7.** Figure 7: Local Mach numbers of the radially inward dust velocity (solid gray) and the root-mean-square of the radial gas velocity (solid purple). The thin gray curves show the dust velocity at different azimuths averaged over the polar angle, and the thick gray curve shows the…

**Figure 9.** Figure 9: Same as Figs. 8a and c, but for s = 0.01 cm (convectiondominated regime). The characteristic convective velocity exceeds the terminal velocity everywhere, such that the dust particles are fully entangled with the convective flow. A sharp increase appears at the inner…

**Figure 8.** Figure 8: Radial profiles of the shell-averaged local Mach number, the Stokes number, and the steady-state dust-to-gas ratio time-averaged over the last ten orbits (top to bottom) for fixed-size particles with s = 1 cm (settling-dominated regime). In panel (a), the dot-dashed bl…

**Figure 10.** Figure 10: Specific collision rate of pebbles computed from Eq. D.1. The recycling flow associated with the midplane outflow suppresses dust accretion onto the core (blue), whereas the inward component of the convective flow enhances dust accretion (orange). The dashed lines m…

**Figure 11.** Figure 11 [PITH_FULL_IMAGE:figures/full_fig_p010_11.png]

**Figure 12.** Figure 12: Schematic illustration of (a) a planet with a non-isolated convective envelope, (b) a planet with a convective envelope effectively isolated from an outer recycling flow, and (c) a planet with a radiative envelope effectively isolated from an outer recycling flow. The…

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Reference graph

Works this paper leans on

300 extracted references · 75 canonical work pages

[1]

A&A , volume=

Gaia Data Release 2 Summary of the contents and survey properties , author=. A&A , volume=. 2018 , publisher=

2018
[2]

ApJ , volume=

Long Baseline Observations of the HD 100546 Protoplanetary Disk with ALMA , author=. ApJ , volume=. 2020 , publisher=

2020
[3]

ApJ , volume=

Kinematic Detections of Protoplanets: A Doppler Flip in the Disk of HD 100546 , author=. ApJ , volume=. 2019 , publisher=

2019
[4]

MNRAS , volume=

The accretion rates and mechanisms of Herbig Ae/Be stars , author=. MNRAS , volume=. 2020 , publisher=

2020
[5]

MNRAS , volume=

A dusty filament and turbulent CO spirals in HD 135344B-SAO 206462 , author=. MNRAS , volume=. 2021 , publisher=

2021
[6]

ApJ , volume=

Kinematic evidence for an embedded protoplanet in a circumstellar disk , author=. ApJ , volume=. 2018 , publisher=

2018
[7]

Evolutionary models and observable properties , author=

Photoevaporation of protoplanetary discs--II. Evolutionary models and observable properties , author=. MNRAS , volume=. 2006 , publisher=

2006
[8]

ApJ , volume=

Turbulent-diffusion mediated CO depletion in weakly turbulent protoplanetary disks , author=. ApJ , volume=. 2017 , publisher=

2017

Show all 300 references

[9]

ApJ , volume=

Transport of CO in protoplanetary disks: Consequences of pebble formation, settling, and radial drift , author=. ApJ , volume=. 2018 , publisher=

2018
[10]

MNRAS , volume=

Planet-forming material in a protoplanetary disc: the interplay between chemical evolution and pebble drift , author=. MNRAS , volume=. 2019 , publisher=

2019
[11]

ApJ , volume=

CO depletion in protoplanetary disks: a unified picture combining physical sequestration and chemical processing , author=. ApJ , volume=. 2020 , publisher=

2020
[12]

ApJ , volume=

A highly settled disk around oph163131 , author=. ApJ , volume=. 2022 , publisher=

2022
[13]

The Gould’s Belt Distances Survey (GOBELINS). I. Trigonometric parallax distances and depth of the ophiuchus complex , author=. ApJ , volume=. 2017 , publisher=

2017
[14]

ApJ , volume=

Gaia-DR2 confirms VLBA parallaxes in Ophiuchus, Serpens, and Aquila , author=. ApJ , volume=. 2018 , publisher=

2018
[15]

The Anatomy of an Unusual Edge-on Protoplanetary Disk. II. Gas temperature and a warm outer region , author=. AJ , volume=. 2021 , publisher=

2021
[16]

Results from continuum data , author=

Observations of edge-on protoplanetary disks with ALMA-I. Results from continuum data , author=. A&A , volume=. 2020 , publisher=

2020
[17]

The Anatomy of an Unusual Edge-on Protoplanetary Disk. I. Dust Settling in a Cold Disk , author=. AJ , volume=. 2021 , publisher=

2021
[18]

MNRAS , volume=

The star formation history and accretion-disc fraction among the K-type members of the Scorpius--Centaurus OB association , author=. MNRAS , volume=. 2016 , publisher=

2016
[19]

Faraday Discussions , volume=

Molecular evolution in planet-forming circumstellar disks , author=. Faraday Discussions , volume=. 1998 , publisher=

1998
[20]

Faraday discussions , volume=

Exploring the origins of carbon in terrestrial worlds , author=. Faraday discussions , volume=. 2014 , publisher=

2014
[21]

Unlocking CO depletion in protoplanetary disks. I. The warm molecular layer , author=. ApJ , volume=. 2018 , publisher=

2018
[22]

A&A , volume=

CO destruction in protoplanetary disk midplanes: Inside versus outside the CO snow surface , author=. A&A , volume=. 2018 , publisher=

2018
[23]

ApJ , volume=

Atmospheres of protoplanetary cores: critical mass for nucleated instability , author=. ApJ , volume=. 2006 , publisher=

2006
[24]

ApJ , volume=

Formation of giant planets: dependences on core accretion rate and grain opacity , author=. ApJ , volume=. 2000 , publisher=

2000
[25]

MNRAS , volume=

Optically thin core accretion: how planets get their gas in nearly gas-free discs , author=. MNRAS , volume=. 2018 , publisher=

2018
[26]

Science Advances , volume=

A pebble accretion model for the formation of the terrestrial planets in the Solar System , author=. Science Advances , volume=. 2021 , publisher=

2021
[27]

Nature Astronomy , volume=

The partitioning of the inner and outer Solar System by a structured protoplanetary disk , author=. Nature Astronomy , volume=. 2020 , publisher=

2020
[28]

Proceedings of the National Academy of Sciences , volume=

Age of Jupiter inferred from the distinct genetics and formation times of meteorites , author=. Proceedings of the National Academy of Sciences , volume=. 2017 , publisher=

2017
[29]

A&A , volume=

Standing on the shoulders of giants-Trojan Earths and vortex trapping in low mass self-gravitating protoplanetary disks of gas and solids , author=. A&A , volume=. 2009 , publisher=

2009
[30]

ApJ , volume=

Including dust coagulation in hydrodynamic models of Protoplanetary disks: Dust Evolution in the Vicinity of a Jupiter-mass Planet , author=. ApJ , volume=. 2019 , publisher=

2019
[31]

AJ , volume=

Probing the protosolar disk using dust filtering at gaps in the early solar system , author=. AJ , volume=. 2019 , publisher=

2019
[32]

arXiv preprint arXiv:1912.12699 , year=

Anticipated Performance of the Square Kilometre Array--Phase 1 (SKA1) , author=. arXiv preprint arXiv:1912.12699 , year=

1912 arXiv
[33]

ApJ , volume=

The Doppler Flip in HD 100546 as a Disk Eruption: The Elephant in the Room of Kinematic Protoplanet Searches , author=. ApJ , volume=. 2022 , publisher=

2022
[34]

Science with a Next Generation Very Large Array , volume=

The ngVLA reference design , author=. Science with a Next Generation Very Large Array , volume=
[35]

arXiv preprint arXiv:2204.04404 , year=

Directly Detecting the Envelopes of Low-mass Planets Embedded In Protoplanetary discs and The Case For TW Hydrae , author=. arXiv preprint arXiv:2204.04404 , year=

arXiv
[36]

Advancing Astrophysics with the Square Kilometre Array , volume=

Advancing astrophysics with the square kilometre array , author=. Advancing Astrophysics with the Square Kilometre Array , volume=. 2015 , organization=

2015
[37]

arXiv preprint arXiv:2001.11076 , year=

The ALMA development program: Roadmap to 2030 , author=. arXiv preprint arXiv:2001.11076 , year=

2001 arXiv
[38]

ApJ , volume=

Investigating the Future Potential of an Upgraded ALMA to Image Planet-forming Disks at Sub-astronomical-unit Scales , author=. ApJ , volume=. 2022 , publisher=

2022
[39]

Characterizing pebble substructure caused by forming planets , author=

Observing protoplanetary discs with the Square Kilometre Array--I. Characterizing pebble substructure caused by forming planets , author=. MNRAS , volume=. 2020 , publisher=

2020
[40]

ApJ , volume=

Investigating the Early Evolution of Planetary Systems with ALMA and the Next Generation Very Large Array , author=. ApJ , volume=. 2018 , publisher=

2018
[41]

ApJ , volume=

Imaging the Dusty Substructures due to Terrestrial Planets in Planet-forming Disks with ALMA and the Next-generation Very Large Array , author=. ApJ , volume=. 2020 , publisher=

2020
[42]

MNRAS , volume=

Extreme pebble accretion in ringed protoplanetary discs , author=. MNRAS , volume=. 2022 , publisher=

2022
[43]

MNRAS , year=

Efficient planet formation by pebble accretion in ALMA rings , author=. MNRAS , year=
[44]

Steady-state model , author=

Dust ring and gap formation by gas flow induced by low-mass planets embedded in protoplanetary disks-I. Steady-state model , author=. A&A , volume=. 2022 , publisher=

2022
[45]

Annual Review of Astronomy and Astrophysics , volume=

Exoplanet statistics and theoretical implications , author=. Annual Review of Astronomy and Astrophysics , volume=. 2021 , publisher=

2021
[46]

Predictions of the WFIRST microlensing survey. I. Bound planet detection rates , author=. ApJS , volume=. 2019 , publisher=

2019
[47]

ApJ , volume=

Magellan adaptive optics imaging of PDS 70: measuring the mass accretion rate of a young giant planet within a gapped disk , author=. ApJ , volume=. 2018 , publisher=

2018
[48]

Nature Astronomy , volume=

Two accreting protoplanets around the young star PDS 70 , author=. Nature Astronomy , volume=. 2019 , publisher=

2019
[49]

ApJ , volume=

Global hydromagnetic simulations of a planet embedded in a dead zone: gap opening, gas accretion, and formation of a protoplanetary jet , author=. ApJ , volume=. 2013 , publisher=

2013
[50]

AJ , volume=

Possible Signatures of Magnetospheric Accretion onto Young Giant Planets , author=. AJ , volume=. 2011 , publisher=

2011
[51]

Searching for H -emitting sources in the gaps of five transitional disks< , author=
[52]

ApJ , volume=

Dust rings as a footprint of planet formation in a protoplanetary disk , author=. ApJ , volume=. 2021 , publisher=

2021
[53]

ApJ , volume=

On mass transport in nonviscous, non-self-gravitating fluid disks , author=. ApJ , volume=
[54]

ApJ , volume=

Zonal flows and long-lived axisymmetric pressure bumps in magnetorotational turbulence , author=. ApJ , volume=. 2009 , publisher=

2009
[55]

ApJ , volume=

Magnetic flux concentration and zonal flows in magnetorotational instability turbulence , author=. ApJ , volume=. 2014 , publisher=

2014
[56]

arXiv preprint arXiv:2201.09241 , year=

A global two-layer radiative transfer model for axisymmetric, shadowed protoplanetary disks , author=. arXiv preprint arXiv:2201.09241 , year=

arXiv
[57]

ApJ , volume=

Nonideal MHD simulation of HL Tau disk: Formation of rings , author=. ApJ , volume=. 2019 , publisher=

2019
[58]

Science , volume=

Spiral density waves in a young protoplanetary disk , author=. Science , volume=. 2016 , publisher=

2016
[59]

ApJ , volume=

Spiral arms in the asymmetrically illuminated disk of MWC 758 and constraints on giant planets , author=. ApJ , volume=. 2012 , publisher=

2012
[60]

ApJ , volume=

Discovery of small-scale spiral structures in the disk of SAO 206462 (HD 135344B): Implications for the physical state of the disk from spiral density wave theory , author=. ApJ , volume=. 2012 , publisher=

2012
[61]

Astronomical Society of the Pacific Conference Series , volume=

Structured Distributions of Gas and Solids in Protoplanetary Disks , author=. Astronomical Society of the Pacific Conference Series , volume=
[62]

Formaldehyde and methanol , author=

A major asymmetric ice trap in a planet-forming disk-I. Formaldehyde and methanol , author=. A&A , volume=. 2021 , publisher=

2021
[63]

A&A , volume=

Asymmetric features in the protoplanetary disk MWC 758 , author=. A&A , volume=. 2015 , publisher=

2015
[64]

ApJ , volume=

SEEDS adaptive optics imaging of the asymmetric transition disk Oph IRS 48 in scattered light , author=. ApJ , volume=. 2015 , publisher=

2015
[65]

ApJ , volume=

Polarized disk emission from Herbig Ae/Be stars observed using Gemini Planet Imager: HD 144432, HD 150193, HD 163296, and HD 169142 , author=. ApJ , volume=. 2017 , publisher=

2017
[66]

A&A , volume=

Shadows and spirals in the protoplanetary disk HD 100453 , author=. A&A , volume=. 2017 , publisher=

2017
[67]

ApJ , volume=

Structures in the protoplanetary disk of HD142527 seen in polarized scattered light , author=. ApJ , volume=. 2014 , publisher=

2014
[68]

3-3700 , author=

Spatial segregation of dust grains in transition disks-SPHERE observations of 2MASS J16083070-3828268 and RXJ1852. 3-3700 , author=. A&A , volume=. 2019 , publisher=

2019
[69]

3--2130 , author=

Variable outer disk shadowing around the Dipper star RXJ1604. 3--2130 , author=. ApJ , volume=. 2018 , publisher=

2018
[70]

A&A , volume=

V1094 Scorpii: A rare giant multi-ringed disk around a T Tauri star , author=. A&A , volume=. 2018 , publisher=

2018
[71]

A&A , volume=

Evidence for a massive dust-trapping vortex connected to spirals-Multi-wavelength analysis of the HD 135344B protoplanetary disk , author=. A&A , volume=. 2018 , publisher=

2018
[72]

ApJ , volume=

The Flared Gas Structure of the Transitional Disk around Sz 91 , author=. ApJ , volume=. 2019 , publisher=

2019
[73]

AJ , volume=

Spiral Structure and Differential Dust Size Distribution in the LKH 330 Disk , author=. AJ , volume=. 2016 , publisher=

2016
[74]

The Disk Substructures at High Angular Resolution Project (DSHARP). X. Multiple rings, a misaligned inner disk, and a bright arc in the disk around the T Tauri star HD 143006 , author=. ApJ , volume=. 2018 , publisher=

2018
[75]

ApJ , volume=

Homogeneous analysis of the dust morphology of transition disks observed with ALMA: investigating dust trapping and the origin of the cavities , author=. ApJ , volume=. 2018 , publisher=

2018
[76]

A&A , volume=

An 80 au cavity in the disk around HD 34282 , author=. A&A , volume=. 2017 , publisher=

2017
[77]

ApJ , volume=

A multi-wavelength analysis of dust and gas in the SR 24S transition disk , author=. ApJ , volume=. 2017 , publisher=

2017
[78]

A&A , volume=

Millimetre spectral indices of transition disks and their relation to the cavity radius , author=. A&A , volume=. 2014 , publisher=

2014
[79]

AJ , volume=

On the diversity of asymmetries in gapped protoplanetary disks , author=. AJ , volume=. 2020 , publisher=

2020
[80]

ApJ , volume=

Planet formation in AB Aurigae: imaging of the inner gaseous spirals observed inside the dust cavity , author=. ApJ , volume=. 2017 , publisher=

2017
[81]

Nature , volume=

Flows of gas through a protoplanetary gap , author=. Nature , volume=. 2013 , publisher=

2013
[82]

PASJ , volume=

Local enhancement of the surface density in the protoplanetary ring surrounding HD 142527 , author=. PASJ , volume=. 2013 , publisher=

2013
[83]

Science , volume=

A major asymmetric dust trap in a transition disk , author=. Science , volume=. 2013 , publisher=

2013
[84]

ApJ , volume=

Dust-depleted Inner Disks in a Large Sample of Transition Disks through Long-baseline ALMA Observations , author=. ApJ , volume=. 2020 , publisher=

2020
[85]

ApJ , volume=

Angular momentum accretion onto a gas giant planet , author=. ApJ , volume=. 2008 , publisher=

2008
[86]

ApJ , volume=

Accretion of solid materials onto circumplanetary disks from protoplanetary disks , author=. ApJ , volume=. 2014 , publisher=

2014
[87]

PASP , volume=

The Keck planet search: detectability and the minimum mass and orbital period distribution of extrasolar planets , author=. PASP , volume=. 2008 , publisher=

2008
[88]

Science , volume=

The occurrence and mass distribution of close-in super-Earths, Neptunes, and Jupiters , author=. Science , volume=. 2010 , publisher=

2010
[89]

ApJ , volume=

The frequency of hot Jupiters orbiting nearby solar-type stars , author=. ApJ , volume=. 2012 , publisher=

2012
[90]

NEPTUNE-SIZE

FAST RISE OF “NEPTUNE-SIZE” PLANETS (4--8 R⊕) FROM P 10 TO 250 DAYS—STATISTICS OF KEPLER PLANET CANDIDATES UP TO 0.75 AU , author=. ApJ , volume=. 2013 , publisher=

2013
[91]

Proceedings of the National Academy of Sciences , volume=

Prevalence of Earth-size planets orbiting Sun-like stars , author=. Proceedings of the National Academy of Sciences , volume=. 2013 , publisher=

2013
[92]

Progress of Theoretical Physics Supplement , volume=

Observed properties of exoplanets: masses, orbits, and metallicities , author=. Progress of Theoretical Physics Supplement , volume=. 2005 , publisher=

2005
[93]

AJ , volume=

The super earth--cold jupiter relations , author=. AJ , volume=. 2018 , publisher=

2018
[94]

AJ , volume=

An excess of Jupiter analogs in super-Earth systems , author=. AJ , volume=. 2019 , publisher=

2019
[95]

Protostars and planets III , pages=

Formation of planetesimals in the solar nebula , author=. Protostars and planets III , pages=
[96]

ApJ , volume=

Low-velocity collisions of centimeter-sized dust aggregates , author=. ApJ , volume=. 2011 , publisher=

2011
[97]

The growth mechanisms of macroscopic bodies in protoplanetary disks , author=. Annu. Rev. Astron. Astrophys. , volume=. 2008 , publisher=

2008
[98]

Mapping the zoo of laboratory collision experiments , author=

The outcome of protoplanetary dust growth: pebbles, boulders, or planetesimals?-I. Mapping the zoo of laboratory collision experiments , author=. A&A , volume=. 2010 , publisher=

2010
[99]

Occurrence, mass distribution and orbital properties of super-Earths and Neptune-mass planets , author=

The HARPS search for southern extra-solar planets XXXIV. Occurrence, mass distribution and orbital properties of super-Earths and Neptune-mass planets , author=. arXiv preprint arXiv:1109.2497 , year=

arXiv
[100]

Progress of Theoretical Physics Supplement , volume=

Structure of the solar nebula, growth and decay of magnetic fields and effects of magnetic and turbulent viscosities on the nebula , author=. Progress of Theoretical Physics Supplement , volume=. 1981 , publisher=

1981
[101]

Reviews of Geophysics , volume=

Fractal aggregates in geophysics , author=. Reviews of Geophysics , volume=. 1991 , publisher=

1991
[102]

Introducing the bouncing barrier , author=

The outcome of protoplanetary dust growth: pebbles, boulders, or planetesimals?-II. Introducing the bouncing barrier , author=. A&A , volume=. 2010 , publisher=

2010
[103]

A&A , volume=

A simple model for the evolution of the dust population in protoplanetary disks , author=. A&A , volume=. 2012 , publisher=

2012
[104]

ApJ , volume=

Sustained magnetorotational turbulence in local simulations of stratified disks with zero net magnetic flux , author=. ApJ , volume=. 2010 , publisher=

2010
[105]

MNRAS , volume=

Emergent mesoscale phenomena in magnetized accretion disc turbulence , author=. MNRAS , volume=. 2012 , publisher=

2012
[106]

MNRAS , volume=

On the width and shape of the corotation region for low-mass planets , author=. MNRAS , volume=. 2009 , publisher=

2009
[107]

Density Waves Excited by Low-mass Planets in Protoplanetary Disks. I. Linear Regime , author=. ApJ , volume=. 2011 , publisher=

2011
[108]

ApJ , volume=

On the migration of protogiant solid cores , author=. ApJ , volume=. 2006 , publisher=

2006
[109]

MNRAS , volume=

Improved torque formula for low-and intermediate-mass planetary migration , author=. MNRAS , volume=. 2017 , publisher=

2017
[110]

A&A , volume=

Recycling of the first atmospheres of embedded planets: Dependence on core mass and optical depth , author=. A&A , volume=. 2022 , publisher=

2022
[111]

MNRAS , volume=

Migrating super-Earths in low-viscosity discs: unveiling the roles of feedback, vortices, and laminar accretion flows , author=. MNRAS , volume=. 2019 , publisher=

2019
[112]

ApJ , keywords =

Disk Frequencies and Lifetimes in Young Clusters. ApJ , keywords =. doi:10.1086/320685 , archivePrefix =. astro-ph/0104347 , primaryClass =

arXiv
[113]

ApJ , volume=

Two-dimensional Study of the Propagation of Planetary Wake and the Indication of Gap Opening in an Inviscid Protoplanetary Disk , author=. ApJ , volume=. 2010 , publisher=

2010
[114]

ApJ , volume=

Accretion of Jupiter-mass planets in the limit of vanishing viscosity , author=. ApJ , volume=. 2014 , publisher=

2014
[115]

arXiv e-prints , keywords =

Visualizing the Kinematics of Planet Formation. arXiv e-prints , keywords =
[116]

ApJ , volume=

Diverse Protoplanetary Disk Morphology Produced by a Jupiter-mass Planet , author=. ApJ , volume=. 2018 , publisher=

2018
[117]

ApJ , volume=

A close-up view of the young circumbinary disk HD 142527 , author=. ApJ , volume=. 2017 , publisher=

2017
[118]

7-213028 , author=

The sizes and depletions of the dust and gas cavities in the transitional disk J160421. 7-213028 , author=. ApJ , volume=. 2017 , publisher=

2017
[119]

ApJ , volume=

New Insights into the Nature of Transition Disks from a Complete Disk Survey of the Lupus Star-forming Region , author=. ApJ , volume=. 2018 , publisher=

2018
[120]

A&A , volume=

Resolved gas cavities in transitional disks inferred from CO isotopologs with ALMA , author=. A&A , volume=. 2016 , publisher=

2016
[121]

ApJ , volume=

ALMA reveals transition of polarization pattern with wavelength in HL Tau’s disk , author=. ApJ , volume=. 2017 , publisher=

2017
[122]

ApJ , volume=

Turbulence in the TW Hya disk , author=. ApJ , volume=. 2018 , publisher=

2018
[123]

ApJ , volume=

A Three-dimensional View of Turbulence: constraints on turbulent motions in the HD 163296 protoplanetary disk using DCO+ , author=. ApJ , volume=. 2017 , publisher=

2017
[124]

ApJ , volume=

No Significant Correlation between Line-emission and Continuum Substructures in the Molecules with ALMA at Planet-forming Scales Program , author=. ApJ , volume=. 2022 , publisher=

2022
[125]

Origin of the Earth and Moon , volume=

Water in the early Earth , author=. Origin of the Earth and Moon , volume=. 2000 , publisher=

2000
[126]

arXiv preprint arXiv:2105.13101 , year=

Evolution of the Water Snow Line in Magnetically Accreting Protoplanetary Disks , author=. arXiv preprint arXiv:2105.13101 , year=

arXiv
[127]

Molecules with ALMA at Planet-forming Scales (MAPS). IV. Emission Surfaces and Vertical Distribution of Molecules , author=. ApJS , volume=. 2021 , publisher=

2021
[128]

Reports on Progress in Physics , volume=

Isotopes in the interstellar medium and circumstellar envelopes , author=. Reports on Progress in Physics , volume=. 1999 , publisher=

1999
[129]

The disk substructures at high angular resolution project (DSHARP). VII. The planet--disk interactions interpretation , author=. ApJ , volume=. 2018 , publisher=

2018
[130]

ApJ , volume=

How efficient is the streaming instability in viscous protoplanetary disks? , author=. ApJ , volume=. 2020 , publisher=

2020
[131]

ApJ , volume=

Streaming Instability in Turbulent Protoplanetary Disks , author=. ApJ , volume=. 2020 , publisher=

2020
[132]

A&A , volume=

How much does turbulence change the pebble isolation mass for planet formation? , author=. A&A , volume=. 2018 , publisher=

2018
[133]

ApJ , volume=

Rossby wave instability of Keplerian accretion disks , author=. ApJ , volume=. 1999 , publisher=

1999
[134]

ApJ , volume=

Parametric study of the Rossby wave instability in a two-dimensional barotropic disk , author=. ApJ , volume=. 2016 , publisher=

2016
[135]

Parametric Study of the Rossby Wave Instability in a Two-dimensional Barotropic Disk. II. Nonlinear Calculations , author=. ApJ , volume=. 2018 , publisher=

2018
[136]

ApJ , volume=

Large-scale Asymmetries in the Transitional Disks of SAO 206462 and SR 21 , author=. ApJ , volume=. 2014 , publisher=

2014
[137]

ApJ , volume=

An azimuthal asymmetry in the LkH 330 disk , author=. ApJ , volume=. 2013 , publisher=

2013
[138]

ApJ , volume=

Mapping the 3D Kinematical Structure of the Gas Disk of HD 169142 , author=. ApJ , volume=. 2021 , publisher=

2021
[139]

MNRAS , volume=

Pebble accretion in Class 0/I YSOs as a possible pathway for early planet formation , author=. MNRAS , volume=. 2019 , publisher=

2019
[140]

ApJ , volume=

Substructure formation in a protostellar disk of L1527 IRS , author=. ApJ , volume=. 2020 , publisher=

2020
[141]

The VLA/ALMA Nascent Disk and Multiplicity (VANDAM) Survey of Orion Protostars. III. Substructures in Protostellar Disks , author=. ApJ , volume=. 2020 , publisher=

2020
[142]

ApJ , volume=

Multiple gaps in the disk of the class i protostar gy 91 , author=. ApJ , volume=. 2018 , publisher=

2018
[143]

ApJ , volume=

Wl 17: A young embedded transition disk , author=. ApJ , volume=. 2017 , publisher=

2017
[144]

ApJ , volume=

New growth mechanism of dust grains in protoplanetary disks with magnetically driven disk winds , author=. ApJ , volume=. 2021 , publisher=

2021
[145]

A&A , volume=

Dust and gas density evolution at a radial pressure bump in protoplanetary disks , author=. A&A , volume=. 2016 , publisher=

2016
[146]

A&A , volume=

Probing the structure of protoplanetary disks: a comparative study of DM Tau, LkCa 15, and MWC 480 , author=. A&A , volume=. 2007 , publisher=

2007
[147]

ApJ , volume=

Resolved images of large cavities in protoplanetary transition disks , author=. ApJ , volume=. 2011 , publisher=

2011
[148]

ApJS , volume=

Pre-main-sequence evolution in the Taurus-Auriga molecular cloud , author=. ApJS , volume=
[149]

ApJ , volume=

A spatially resolved au-scale inner disk around DM Tau , author=. ApJ , volume=. 2018 , publisher=

2018
[150]

A&A , volume=

Accretion of eroding pebbles and planetesimals in planetary envelopes , author=. A&A , volume=. 2020 , publisher=

2020
[151]

MNRAS , volume=

Are pebble pile planetesimals doomed? , author=. MNRAS , volume=. 2019 , publisher=

2019
[152]

Journal of Geophysical Research: Atmospheres , volume=

A simple expression for wind erosion threshold friction velocity , author=. Journal of Geophysical Research: Atmospheres , volume=. 2000 , publisher=

2000
[153]

A&A , volume=

Closed-form expressions for particle relative velocities induced by turbulence , author=. A&A , volume=. 2007 , publisher=

2007
[154]

A&A , volume=

Large grains in the disk of CQ Tau , author=. A&A , volume=. 2003 , publisher=

2003
[155]

ApJ , volume=

The radial distribution of dust particles in the HL Tau Disk from ALMA and VLA observations , author=. ApJ , volume=. 2019 , publisher=

2019
[156]

ApJ , volume=

The 3D Dust and Opacity Distribution of Protoplanets in Multifluid Global Simulations , author=. ApJ , volume=. 2022 , publisher=

2022
[157]

Three-dimensional interaction between a planet and an isothermal gaseous disk. I. Corotation and Lindblad torques and planet migration , author=. ApJ , volume=. 2002 , publisher=

2002
[158]

icarus , volume=

Density waves in the solar nebula: Diffential Lindblad torque , author=. icarus , volume=. 1986 , publisher=

1986
[159]

Nature , volume=

Meridional flows in the disk around a young star , author=. Nature , volume=. 2019 , publisher=

2019
[160]

Molecules with ALMA at Planet-forming Scales (MAPS). XV. Tracing protoplanetary disk structure within 20 au , author=. ApJS , volume=. 2021 , publisher=

2021
[161]

MNRAS , volume=

Migrating low-mass planets in inviscid dusty protoplanetary discs , author=. MNRAS , volume=. 2020 , publisher=

2020
[162]

MNRAS , volume=

Vortex instabilities triggered by low-mass planets in pebble-rich, inviscid protoplanetary discs , author=. MNRAS , volume=. 2019 , publisher=

2019
[163]

ApJ , volume=

The Irradiation Instability of Protoplanetary Disks , author=. ApJ , volume=. 2021 , publisher=

2021
[164]

ApJ , volume=

Thermal waves in irradiated protoplanetary disks , author=. ApJ , volume=. 2008 , publisher=

2008
[165]

ApJ , volume=

Dust Pileup at the Dead-zone Inner Edge and Implications for the Disk Shadow , author=. ApJ , volume=. 2019 , publisher=

2019
[166]

ApJ , volume=

Thermal Wave Instability as an Origin of Gap and Ring Structures in Protoplanetary Disks , author=. ApJ , volume=. 2021 , publisher=

2021
[167]

ApJ , volume=

Temperature, Mass, and Turbulence: A Spatially Resolved Multiband Non-LTE Analysis of CS in TW Hya , author=. ApJ , volume=. 2018 , publisher=

2018
[168]

ApJ , volume=

Weak turbulence in the HD 163296 protoplanetary disk revealed by ALMA CO observations , author=. ApJ , volume=. 2015 , publisher=

2015
[169]

MNRAS , volume=

On the vertical shear instability in magnetized protoplanetary discs , author=. MNRAS , volume=. 2021 , publisher=

2021
[170]

ApJ , volume=

Global Simulations of the Vertical Shear Instability with Nonideal Magnetohydrodynamic Effects , author=. ApJ , volume=. 2020 , publisher=

2020
[171]

ApJ , volume=

Gap opening in 3D: single-planet gaps , author=. ApJ , volume=. 2016 , publisher=

2016
[172]

ApJ , volume=

Effects of Dust Evolution on the Vertical Shear Instability in the Outer Regions of Protoplanetary Disks , author=. ApJ , volume=. 2021 , publisher=

2021
[173]

A&A , volume=

Steady state by recycling prevents premature collapse of protoplanetary atmospheres , author=. A&A , volume=. 2021 , publisher=

2021
[174]

Molecules with ALMA at Planet-forming Scales (MAPS). V. CO Gas Distributions , author=. ApJS , volume=. 2021 , publisher=

2021
[175]

ApJ , volume=

Ring Formation by Coagulation of Dust Aggregates in the Early Phase of Disk Evolution around a Protostar , author=. ApJ , volume=. 2021 , publisher=

2021
[176]

On the horseshoe drag of a low-mass planet. II. Migration in adiabatic disks , author=. ApJ , volume=. 2009 , publisher=

2009
[177]

A&A , volume=

Growing and moving low-mass planets in non-isothermal disks , author=. A&A , volume=. 2008 , publisher=

2008
[178]

ApJ , volume=

Formation, early evolution, and gravitational stability of protoplanetary disks , author=. ApJ , volume=
[179]

Progress of Theoretical Physics , volume=

Growth of solid particles in the primordial solar nebula , author=. Progress of Theoretical Physics , volume=. 1970 , publisher=

1970
[180]

ApJ , volume=

Evolution of snow line in optically thick protoplanetary disks: effects of water ice opacity and dust grain size , author=. ApJ , volume=. 2011 , publisher=

2011
[181]

ApJ , volume=

The effect of internal dissipation and surface irradiation on the structure of disks and the location of the snow line around Sun-like stars , author=. ApJ , volume=. 2007 , publisher=

2007
[182]

ApJ , volume=

How empty are disk gaps opened by giant planets? , author=. ApJ , volume=. 2014 , publisher=

2014
[183]

ApJ , volume=

Gap opening by extremely low-mass planets in a viscous disk , author=. ApJ , volume=. 2013 , publisher=

2013
[184]

Icarus , volume=

On the width and shape of gaps in protoplanetary disks , author=. Icarus , volume=. 2006 , publisher=

2006
[185]

MNRAS , volume=

The migration and growth of protoplanets in protostellar discs , author=. MNRAS , volume=. 2000 , publisher=

2000
[186]

MNRAS , volume=

Mass flow and accretion through gaps in accretion discs , author=. MNRAS , volume=. 1999 , publisher=

1999
[187]

Annual Review of Astronomy and Astrophysics , volume=

Planet-disk interaction and orbital evolution , author=. Annual Review of Astronomy and Astrophysics , volume=. 2012 , publisher=

2012
[188]

ApJ , volume=

Planet migration and gap formation by tidally induced shocks , author=. ApJ , volume=. 2002 , publisher=

2002
[189]

ApJ , volume=

Planetary torques as the viscosity of protoplanetary disks , author=. ApJ , volume=. 2001 , publisher=

2001
[190]

ApJ , volume=

The Growth of Protoplanets via the Accretion of Small Bodies in Disks Perturbed by the Planetary Gravity , author=. ApJ , volume=. 2021 , publisher=

2021
[191]

A&A , volume=

Oscillatory migration of accreting protoplanets driven by a 3D distortion of the gas flow , author=. A&A , volume=. 2019 , publisher=

2019
[192]

A&A , volume=

How do giant planetary cores shape the dust disk?-hl tauri system , author=. A&A , volume=. 2015 , publisher=

2015
[193]

ApJ , volume=

Impacts of dust feedback on a dust ring induced by a planet in a protoplanetary disk , author=. ApJ , volume=. 2018 , publisher=

2018
[194]

A&A , volume=

The effect of a planet on the dust distribution in a 3D protoplanetary disk , author=. A&A , volume=. 2007 , publisher=

2007
[195]

Observability with ALMA , author=

Planet gaps in the dust layer of 3D protoplanetary disks-II. Observability with ALMA , author=. A&A , volume=. 2012 , publisher=

2012
[196]

MNRAS , volume=

Tidal torques on accretion discs in binary systems with extreme mass ratios , author=. MNRAS , volume=. 1979 , publisher=

1979
[197]

II-Self-consistent nonlinear interaction , author=

On the tidal interaction between protoplanets and the primordial solar nebula. II-Self-consistent nonlinear interaction , author=. ApJ , volume=
[198]

Nature , volume=

Imaging the water snow-line during a protostellar outburst , author=. Nature , volume=. 2016 , publisher=

2016
[199]

The Disk Substructures at High Angular Resolution Program (DSHARP). VIII. The Rich Ringed Substructures in the AS 209 Disk , author=. ApJ , volume=. 2018 , publisher=

2018
[200]

ApJ , volume=

Scattered light from dust in the cavity of the V4046 Sgr transition disk , author=. ApJ , volume=. 2015 , publisher=

2015
[201]

Disks around T Tauri stars with SPHERE (DARTTS-S). I. SPHERE/IRDIS polarimetric imaging of eight prominent T Tauri disks , author=. ApJ , volume=. 2018 , publisher=

2018
[202]

ApJ , volume=

Gaps in the HD 169142 protoplanetary disk revealed by polarimetric imaging: signs of ongoing planet formation? , author=. ApJ , volume=. 2013 , publisher=

2013
[203]

ApJ , volume=

Secular Gravitational Instability of Drifting Dust in Protoplanetary Disks: Formation of Dusty Rings without Significant Gas Substructures , author=. ApJ , volume=. 2020 , publisher=

2020
[204]

non-ideal mhd case , author=

Global simulations of protoplanetary disks with net magnetic flux-i. non-ideal mhd case , author=. A&A , volume=. 2017 , publisher=

2017
[205]

A&A , volume=

Planetesimal formation starts at the snow line , author=. A&A , volume=. 2017 , publisher=

2017
[206]

A&A , volume=

Close-in planetesimal formation by pile-up of drifting pebbles , author=. A&A , volume=. 2016 , publisher=

2016
[207]

MNRAS , volume=

Self-induced dust traps: overcoming planet formation barriers , author=. MNRAS , volume=. 2017 , publisher=

2017
[208]

Axisymmetric resistive MHD simulations , author=

Rings and gaps produced by variable magnetic disc winds and avalanche accretion streams--I. Axisymmetric resistive MHD simulations , author=. MNRAS , volume=. 2017 , publisher=

2017
[209]

MNRAS , volume=

The formation of rings and gaps in magnetically coupled disc-wind systems: ambipolar diffusion and reconnection , author=. MNRAS , volume=. 2018 , publisher=

2018
[210]

MNRAS , volume=

ALMA images of discs: are all gaps carved by planets? , author=. MNRAS , volume=. 2015 , publisher=

2015
[211]

ApJ , volume=

Protoplanetary Disks in Ophiuchus as Seen from ALMA , author=. ApJ , volume=. 2017 , publisher=

2017
[212]

PASJ , volume=

Mass constraint for a planet in a protoplanetary disk from the gap width , author=. PASJ , volume=. 2016 , publisher=

2016
[213]

ApJ , volume=

Mass estimates of a giant planet in a protoplanetary disk from the gap structures , author=. ApJ , volume=. 2015 , publisher=

2015
[214]

PASJ , volume=

Non-linear development of secular gravitational instability in protoplanetary disks , author=. PASJ , volume=. 2018 , publisher=

2018
[215]

ApJ , volume=

Revised description of dust diffusion and a new instability creating multiple rings in protoplanetary disks , author=. ApJ , volume=. 2019 , publisher=

2019
[216]

ApJ , volume=

Evidence of fast pebble growth near condensation fronts in the HL Tau protoplanetary disk , author=. ApJ , volume=. 2015 , publisher=

2015
[217]

ApJ , volume=

Sintering-induced dust ring formation in protoplanetary disks: Application to the HL tau disk , author=. ApJ , volume=. 2016 , publisher=

2016
[218]

A&A , volume=

Gaps, rings, and non-axisymmetric structures in protoplanetary disks-From simulations to ALMA observations , author=. A&A , volume=. 2015 , publisher=

2015
[219]

ApJ , volume=

Dust and gas in the disk of HL Tauri: surface density, dust settling, and dust-to-gas ratio , author=. ApJ , volume=. 2015 , publisher=

2015
[220]

ApJ , volume=

ALMA Observations of Elias 2--24: A Protoplanetary Disk with Multiple Gaps in the Ophiuchus Molecular Cloud , author=. ApJ , volume=. 2017 , publisher=

2017
[221]

ApJ , volume=

Dual-wavelength ALMA observations of dust rings in protoplanetary disks , author=. ApJ , volume=. 2020 , publisher=

2020
[222]

ApJ , volume=

Protoplanetary disk rings and gaps across ages and luminosities , author=. ApJ , volume=. 2019 , publisher=

2019
[223]

ApJ , volume=

A gap with a deficit of large grains in the protoplanetary disk around TW Hya , author=. ApJ , volume=. 2016 , publisher=

2016
[224]

ApJ , volume=

ALMA Observations of a Gap and a Ring in the Protoplanetary Disk around TW Hya , author=. ApJ , volume=. 2016 , publisher=

2016
[225]

ApJ , volume=

High-Resolution Millimeter Imaging of the CI Tau Protoplanetary Disk: A Massive Ensemble of Protoplanets from 0.1 to 100 au , author=. ApJ , volume=. 2018 , publisher=

2018
[226]

The disk substructures at high angular resolution project (DSHARP). I. Motivation, sample, calibration, and overview , author=. ApJ , volume=. 2018 , publisher=

2018
[227]

The disk substructures at high angular resolution project (DSHARP). II. Characteristics of annular substructures , author=. ApJ , volume=. 2018 , publisher=

2018
[228]

The disk substructures at high angular resolution project (DSHARP). III. Spiral structures in the millimeter continuum of the Elias 27, IM Lup, and WaOph 6 disks , author=. ApJ , volume=. 2018 , publisher=

2018
[229]

A&A , volume=

ALMA continuum observations of the protoplanetary disk AS 209-Evidence of multiple gaps opened by a single planet , author=. A&A , volume=. 2018 , publisher=

2018
[230]

ApJ , volume=

CO and dust properties in the TW Hya disk from high-resolution ALMA observations , author=. ApJ , volume=. 2018 , publisher=

2018
[231]

ApJ , volume=

Ringed substructure and a gap at 1 au in the nearest protoplanetary disk , author=. ApJ , volume=. 2016 , publisher=

2016
[232]

MNRAS , volume=

A ring-like concentration of mm-sized particles in Sz 91 , author=. MNRAS , volume=. 2016 , publisher=

2016
[233]

3-3255-High contrast imaging with VLT/SPHERE , author=

Multiple rings in the transition disk and companion candidates around RX J1615. 3-3255-High contrast imaging with VLT/SPHERE , author=. A&A , volume=. 2016 , publisher=

2016
[234]

A&A , volume=

Direct detection of scattered light gaps in the transitional disk around HD 97048 with VLT/SPHERE , author=. A&A , volume=. 2016 , publisher=

2016
[235]

Physical Review Letters , volume=

Ringed structures of the HD 163296 protoplanetary disk revealed by ALMA , author=. Physical Review Letters , volume=. 2016 , publisher=

2016
[236]

ApJ , volume=

Three radial gaps in the disk of TW Hydrae imaged with SPHERE , author=. ApJ , volume=. 2017 , publisher=

2017
[237]

A&A , volume=

Cavity and other radial substructures in the disk around HD 97048 , author=. A&A , volume=. 2017 , publisher=

2017
[238]

A&A , volume=

ALMA unveils rings and gaps in the protoplanetary system HD 169142: signatures of two giant protoplanets , author=. A&A , volume=. 2017 , publisher=

2017
[239]

MNRAS , volume=

An opening criterion for dust gaps in protoplanetary discs , author=. MNRAS , volume=. 2017 , publisher=

2017
[240]

A&A , volume=

Dust accretion onto high-mass planets , author=. A&A , volume=. 2007 , publisher=

2007
[241]

MNRAS , volume=

Morphological signatures induced by dust back reaction in discs with an embedded planet , author=. MNRAS , volume=. 2020 , publisher=

2020
[242]

A&A , volume=

Planet formation by pebble accretion in ringed disks , author=. A&A , volume=. 2020 , publisher=

2020
[243]

A hybrid accretion scenario , author=

Giant planet formation at the pressure maxima of protoplanetary disks-II. A hybrid accretion scenario , author=. A&A , volume=. 2020 , publisher=

2020
[244]

MNRAS , volume=

On the origin of horseshoes in transitional discs , author=. MNRAS , volume=. 2017 , publisher=

2017
[245]

MNRAS , volume=

Dust filtration at gap edges: implications for the spectral energy distributions of discs with embedded planets , author=. MNRAS , volume=. 2006 , publisher=

2006
[246]

arXiv preprint arXiv:2009.04775 , year=

Concurrent effects of gas drag and planet migration on pebble accretion , author=. arXiv preprint arXiv:2009.04775 , year=

2009 arXiv
[247]

A&A , volume=

Dust trapping around Lagrangian points in protoplanetary disks , author=. A&A , volume=. 2020 , publisher=

2020
[248]

Annual Review of Astronomy and Astrophysics , volume=

Observations of protoplanetary disk structures , author=. Annual Review of Astronomy and Astrophysics , volume=. 2020 , publisher=

2020
[249]

MNRAS , volume=

Two mechanisms for dust gap opening in protoplanetary discs , author=. MNRAS , volume=. 2016 , publisher=

2016
[250]

MNRAS , volume=

The minimum mass of detectable planets in protoplanetary discs and the derivation of planetary masses from high-resolution observations , author=. MNRAS , volume=. 2016 , publisher=

2016
[251]

The Disk Substructures at High Angular Resolution Project (DSHARP). IX. A high-definition study of the HD 163296 planet-forming disk , author=. ApJ , volume=. 2018 , publisher=

2018
[252]

ApJ , volume=

ALMA Observations of the Asymmetric Dust Disk around DM Tau , author=. ApJ , volume=. 2021 , publisher=

2021
[253]

ApJ , volume=

Estimate on Dust Scale Height from the ALMA Dust Continuum Image of the HD 163296 Protoplanetary Disk , author=. ApJ , volume=. 2021 , publisher=

2021
[254]

A&A , volume=

Ring shaped dust accumulation in transition disks , author=. A&A , volume=. 2012 , publisher=

2012
[255]

arXiv preprint arXiv:2103.02392 , year=

A super-resolution analysis of the DSHARP survey: Substructure is common in the inner 30 au , author=. arXiv preprint arXiv:2103.02392 , year=

arXiv
[256]

Puffed-up Edges of Planet-opened Gaps in Protoplanetary Disks. I. Hydrodynamic Simulations , author=. ApJ , volume=. 2021 , publisher=

2021
[257]

The disk substructures at high angular resolution project (DSHARP). VI. Dust trapping in thin-ringed protoplanetary disks , author=. ApJ , volume=. 2018 , publisher=

2018
[258]

AJ , volume=

Probing the Protosolar disk using dust filtering at gaps in the Early Solar System , author=. AJ , volume=. 2019 , publisher=

2019
[259]

ApJ , volume=

Dust filtration by planet-induced gap edges: implications for transitional disks , author=. ApJ , volume=. 2012 , publisher=

2012
[260]

arXiv preprint arXiv:2103.10177 , year=

First 3-D grid-based gas-dust simulations of circumstellar disks with an embedded planet , author=. arXiv preprint arXiv:2103.10177 , year=

arXiv
[261]

Model properties , author=

Global MHD simulations of stratified and turbulent protoplanetary discs-I. Model properties , author=. A&A , volume=. 2006 , publisher=

2006
[262]

ApJ , volume=

Characterizing the variable dust permeability of planet-induced gaps , author=. ApJ , volume=. 2018 , publisher=

2018
[263]

MNRAS , volume=

Increased isolation mass for pebble accreting planetary cores in pressure maxima of protoplanetary discs , author=. MNRAS , volume=. 2021 , publisher=

2021
[264]

MNRAS , volume=

Dust trapping by spiral arms in gravitationally unstable protostellar discs , author=. MNRAS , volume=. 2015 , publisher=

2015
[265]

MNRAS , volume=

Rings and gaps in the disc around Elias 24 revealed by ALMA , author=. MNRAS , volume=. 2018 , publisher=

2018
[266]

MNRAS , volume=

Enforcing dust mass conservation in 3D simulations of tightly coupled grains with the PHANTOM SPH code , author=. MNRAS , volume=. 2018 , publisher=

2018
[267]

A&A , volume=

Ring structure in the MWC 480 disk revealed by ALMA , author=. A&A , volume=. 2019 , publisher=

2019
[268]

ApJ , volume=

Gaps and rings in an ALMA survey of disks in the Taurus star-forming region , author=. ApJ , volume=. 2018 , publisher=

2018
[269]

MNRAS , volume=

The newborn planet population emerging from ring-like structures in discs , author=. MNRAS , volume=. 2019 , publisher=

2019
[270]

MNRAS , volume=

A dust and gas cavity in the disc around CQ Tau revealed by ALMA , author=. MNRAS , volume=. 2019 , publisher=

2019
[271]

A&A , volume=

Observational constraints on dust disk sizes in tidally truncated protoplanetary disks in multiple systems in the Taurus region , author=. A&A , volume=. 2019 , publisher=

2019
[272]

ApJ , volume=

Rapid Formation of Jupiter and Wide-orbit Exoplanets in Disks with Pressure Bumps , author=. ApJ , volume=. 2021 , publisher=

2021
[273]

A&A , volume=

A tunnel and a traffic jam: How transition disks maintain a detectable warm dust component despite the presence of a large planet-carved gap , author=. A&A , volume=. 2016 , publisher=

2016
[274]

A&A , volume=

Dust flow in gas disks in the presence of embedded planets , author=. A&A , volume=. 2006 , publisher=

2006
[275]

ApJ , volume=

Dust-trapping vortices and a potentially planet-triggered spiral wake in the pre-transitional disk of v1247 orionis , author=. ApJ , volume=. 2017 , publisher=

2017
[276]

A&A , volume=

Planets opening dust gaps in gas disks , author=. A&A , volume=. 2004 , publisher=

2004
[277]

Particle concentration at planet-induced gap edges and vortices. I. Inviscid three-dimensional hydro disks , author=. ApJ , volume=. 2014 , publisher=

2014
[278]

Hydrodynamical simulations of T Tauri disks , author=

Planet gaps in the dust layer of 3D protoplanetary disks-I. Hydrodynamical simulations of T Tauri disks , author=. A&A , volume=. 2010 , publisher=

2010
[279]

MNRAS , volume=

On the accumulation of planetesimals near disc gaps created by protoplanets , author=. MNRAS , volume=. 2012 , publisher=

2012
[280]

ApJ , volume=

Multiple disk gaps and rings generated by a single super-earth , author=. ApJ , volume=. 2017 , publisher=

2017
[281]

AJ , volume=

Dust unveils the formation of a mini-Neptune planet in a protoplanetary ring , author=. AJ , volume=. 2019 , publisher=

2019
[282]

ApJ , volume=

Planet formation signposts: observability of circumplanetary disks via gas kinematics , author=. ApJ , volume=. 2015 , publisher=

2015
[283]

Multiple disk gaps and rings generated by a single super-Earth. II. Spacings, depths, and number of gaps, with application to real systems , author=. ApJ , volume=. 2018 , publisher=

2018
[284]

MNRAS , volume=

Spiral arms in scattered light images of protoplanetary discs: are they the signposts of planets? , author=. MNRAS , volume=. 2015 , publisher=

2015
[285]

Observational signatures of planets in protoplanetary disks. I. Gaps opened by single and multiple young planets in disks , author=. ApJ , volume=. 2015 , publisher=

2015
[286]

ApJ , volume=

Attenuation of millimeter emission from circumstellar disks induced by the rapid dust accretion , author=. ApJ , volume=. 2005 , publisher=

2005
[287]

A&A , volume=

Growth after the streaming instability-From planetesimal accretion to pebble accretion , author=. A&A , volume=. 2019 , publisher=

2019
[288]

Influences of protoplanet-induced three-dimensional gas flow on pebble accretion. II. Headwind regime. A&A , keywords =. doi:10.1051/0004-6361/202039153 , archivePrefix =. 2009.07636 , primaryClass =

2009 arXiv
[289]

ApJ , volume=

A resolved census of millimeter emission from taurus multiple star systems , author=. ApJ , volume=. 2012 , publisher=

2012
[290]

AJ , volume=

Symplectic maps for the n-body problem-stability analysis , author=. AJ , volume=
[291]

arXiv preprint astro-ph/9403057 , year=

Long-term planetary integration with individual time steps , author=. arXiv preprint astro-ph/9403057 , year=

arXiv
[292]

Inc., Richmond, VA , volume=

Fundamentals of celestial mechanics, Willmann-Bell , author=. Inc., Richmond, VA , volume=
[293]

ApJ , volume=

Multiple Spiral Arms in Protoplanetary Disks: Linear Theory , author=. ApJ , volume=. 2019 , publisher=

2019
[294]

ApJ , volume=

On the Dust Signatures Induced by Eccentric Super-Earths in Protoplanetary Disks , author=. ApJ , volume=. 2019 , publisher=

2019
[295]

ApJ , volume=

Predicting the observational signature of migrating Neptune-sized planets in low-viscosity disks , author=. ApJ , volume=. 2019 , publisher=

2019
[296]

A&A , volume=

Vertical shear instability in accretion disc models with radiation transport , author=. A&A , volume=. 2014 , publisher=

2014
[297]

On the early evolution of forming Jovian planets. I. Initial conditions, systematics, and qualitative comparisons to theory , author=. ApJ , volume=. 2003 , publisher=

2003
[298]

ApJ , volume=

On the planetary interpretation of multiple gaps and rings in protoplanetary disks seen by ALMA , author=. ApJ , volume=. 2019 , publisher=

2019
[299]

ApJ , volume=

Dynamics of circumstellar disks , author=. ApJ , volume=. 1998 , publisher=

1998
[300]

AJ , volume=

Satellite dynamics on the Laplace surface , author=. AJ , volume=. 2009 , publisher=

2009

Pith tools

Reviewed August 8, 2026 · model on record in the stance chip above.

[1] [1]

A&A , volume=

Gaia Data Release 2 Summary of the contents and survey properties , author=. A&A , volume=. 2018 , publisher=

2018

[2] [2]

ApJ , volume=

Long Baseline Observations of the HD 100546 Protoplanetary Disk with ALMA , author=. ApJ , volume=. 2020 , publisher=

2020

[3] [3]

ApJ , volume=

Kinematic Detections of Protoplanets: A Doppler Flip in the Disk of HD 100546 , author=. ApJ , volume=. 2019 , publisher=

2019

[4] [4]

MNRAS , volume=

The accretion rates and mechanisms of Herbig Ae/Be stars , author=. MNRAS , volume=. 2020 , publisher=

2020

[5] [5]

MNRAS , volume=

A dusty filament and turbulent CO spirals in HD 135344B-SAO 206462 , author=. MNRAS , volume=. 2021 , publisher=

2021

[6] [6]

ApJ , volume=

Kinematic evidence for an embedded protoplanet in a circumstellar disk , author=. ApJ , volume=. 2018 , publisher=

2018

[7] [7]

Evolutionary models and observable properties , author=

Photoevaporation of protoplanetary discs--II. Evolutionary models and observable properties , author=. MNRAS , volume=. 2006 , publisher=

2006

[8] [8]

ApJ , volume=

Turbulent-diffusion mediated CO depletion in weakly turbulent protoplanetary disks , author=. ApJ , volume=. 2017 , publisher=

2017