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Wind-launching disks: planet-opened gaps act as porous filters, not absolute barriers, for radial gas and dust transport.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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2026-08-01 10:36 UTC pith:WQ4GTVVQ

load-bearing objection A genuine step beyond hydro gap-filtering studies — dust transport in 3D MHD wind-launching disks with planets — but the leaky-gap headline depends on an untested ionization boost and unresolved inflow channels, so it is plausible rather than robust. the 3 major comments →

arxiv 2607.20158 v1 pith:WQ4GTVVQ submitted 2026-07-22 astro-ph.EP

Dust and Gas Transport in Substructured Nonideal MHD Wind-Launching Disks with Embedded Planets

Chun-Yen Hsu , Zhi-Yun Li , Xiao Hu , Yisheng Tu , Min-Kai Lin This is my paper
classification astro-ph.EP
keywords protoplanetary disksnonideal MHDdisk windsplanet-disk interactiondust transportgap permeabilitypebble isolationdisk chemistry
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

Using 3D nonideal magnetohydrodynamic simulations of wind-launching disks with embedded planets, this paper tries to establish that disk substructures of both magnetic and planetary origin regulate, but do not halt, radial gas and dust transport. A Jupiter-mass planet opens a deep gap and temporarily reverses inward flow at its outer edge, yet wind-driven accretion persists and reorganizes into localized, azimuthally intermittent inflow channels that leak material across the gap. Dust filtering is strongly size-dependent: small grains cross with the gas, while millimeter-sized grains are trapped outside the planet, so the planet acts as an efficient but incomplete filter. If this picture is right, observed inner-disk volatile compositions and the meteoritic non-carbonaceous/carbonaceous dichotomy can be explained without an impermeable Jovian barrier, and pebble isolation should be viewed as a gradual, flow-dependent process rather than a sharp cutoff.

Core claim

The core discovery is the leaky-gap scenario: in a globally magnetized, wind-launching disk, a gap carved by a Jupiter-mass planet remains intrinsically time-dependent and partially permeable. The planet reshapes, rather than replaces, the magnetically driven flow: spiral shocks suppress or reverse inward motion along the arms, but inter-arm regions continue to accrete under magnetic stresses, forming spiral-shaped inflow channels that intermittently penetrate the gap. Gas and small grains follow these channels; large grains are efficiently filtered at the outer pressure maximum, but even 1–10 mm grains can cross intermittently. The authors further find that MHD-generated rings and gaps modu

What carries the argument

The load-bearing mechanism is the wind-driven accretion stream concentrated in a thin midplane current sheet, the layer where the radial and azimuthal magnetic fields reverse sign, which coexists with the planet's spiral shocks. In the Jupiter-mass run, the planet's torque opposes this stream along spiral arms, but the stream is not destroyed; it is warped and fragmented, then re-emerges in inter-arm regions as azimuthally intermittent, vertically displaced inflow channels. These channels are what make the gap porous. In the dust sector, aerodynamic coupling to this structured flow produces the size-dependent filtering: small grains are carried on the vertically extended flow, while large gr

Load-bearing premise

The main load-bearing assumption is that the disk surface is strongly enough ionized to keep the magnetized wind and its midplane accretion streams alive, enforced through an ad hoc enhancement of the nonideal diffusivities above the disk, while rapid cooling keeps the disk nearly isothermal; if the real ionization is weaker, the planet's gap could be a much more effective barrier.

What would settle it

Run the same Jupiter-mass setup with a self-consistent ionization calculation that omits the ad hoc diffusivity enhancement, and repeat at twice the resolution; if the azimuthally and time-averaged inward gas mass flux across the gap drops to zero over many orbits, with no inter-arm inflow channels surviving, the leaky-gap claim is falsified.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • Neither wind-driven rings and gaps nor planet-opened gaps, on their own, should be treated as transport barriers; axisymmetric surface-density depressions do not imply a halt of radial flow.
  • Inner disks can receive volatile-rich solids both before gap opening and through later leakage, so diverse inner-disk molecular compositions can coexist with outer substructures.
  • The non-carbonaceous/carbonaceous meteorite dichotomy can be set up without a perfectly impermeable Jupiter; early mixing plus later size-dependent filtration suffices.
  • Pebble isolation is not a sharp threshold: planets near or above the classical isolation mass can still receive inward pebble flux, shifting the effective isolation threshold to higher masses in magnetically driven disks.
  • Circumplanetary disks of giant planets can be depleted in large grains, down to roughly 20% of their initial abundance, because delivery through vertically structured accretion flows preferentially carries small grains.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • An observational extension: if the leaky-gap mechanism is real, high-resolution dust-continuum and molecular-line maps of disks with giant-planet gaps should show azimuthal asymmetries, patchy dust rings, and intermittent bridges of material rather than smooth, sharply bounded gap edges.
  • A modeling extension: chemical-evolution and isotopic-mixing models of planet-forming disks should replace the open-versus-closed barrier dichotomy with a time-dependent, size-dependent leakage prescription; the difference will matter for predicted carbon-to-oxygen ratios and volatile enrichment timescales.
  • A dynamical extension: the result implies that the classical pebble isolation mass is an upper envelope set in hydrodynamic disks; in wind-launching disks the effective isolation threshold depends on magnetic field strength and ionization, so two disks with identical planet masses could filter solids very differently.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 4 minor

Summary. The paper presents global 3D non-ideal MHD simulations of wind-launching protoplanetary disks with embedded planets of 0.01, 0.1, and 1 Jupiter masses, both gas-only and with five dust bins spanning 0.1 mm to 10 mm. The central claim is that neither MHD-generated rings/gaps nor planet-opened gaps act as absolute barriers to radial gas and dust transport. In the Jupiter-mass case, the gap is partially permeable: after an early suppression, localized, azimuthally intermittent inflow channels develop and allow continued inward transport, with small grains crossing with the gas while larger grains are partially filtered and trapped exterior to the planet. The authors interpret this as a 'leaky gap' scenario and apply it to inner-disk volatile delivery, the NC/CC meteoritic dichotomy, and pebble isolation.

Significance. If correct, this is an important advance: it moves the discussion of gap permeability from viscous/turbulent disk parameterizations to self-consistent non-ideal MHD wind-launching disks, where the leak is produced by time-dependent, non-axisymmetric magnetic-stress-driven accretion streams rather than prescribed diffusion. The paper's diagnostics (integrated mass crossing in Figs. 3 and 12) are well suited to the claim, and no parameters are fitted to the target conclusions; the leaky-gap behavior emerges from the dynamics. The main weaknesses—the ad hoc f(θ) ionization boost and the absence of any resolution study—are specific and testable. The central claim is plausible but not yet robust.

major comments (3)
  1. [Sec. 2.5, Eq. (16)] The leaky-gap conclusion in Secs. 3.3 and 4.3 relies on the persistence of wind-driven accretion streams in the inter-arm regions. These streams depend on the magnetic coupling that Eq. (16) artificially increases in the atmosphere by reducing the Ohmic and ambipolar diffusivities. No run with f≡1 (or with a different boost amplitude) is presented. If the actual ionization environment produces a weaker wind, the Jovian gap could be a much more effective barrier. A sensitivity run, or a quantitative physical justification for the adopted f(θ) profile, is needed to support the headline claim.
  2. [Sec. 2.1 and Figs. 4, 13] The leak is carried by thin, vertically displaced accretion channels that are resolved only by the SMR grid. The third refinement level provides approximately 12.6 cells per scale height, and the finest level is confined to ±0.05 rad around the planet, so it does not cover the inter-arm channels that appear in Figs. 4 and 13. No convergence study is reported. Without a resolution test (at least one coarser and one finer global refinement), it remains uncertain whether the intermittent inflow channels are physical or partly numerical artifacts. This is load-bearing for the 'no absolute barrier' conclusion.
  3. [Sec. 5.2] The paper itself cautions that the pre-loading of large grains in the inner disk is influenced by the idealized insertion of a fully formed giant planet into an initially undepleted disk. This limitation directly affects the quantitative support for the 'efficient but incomplete filter' claim and its NC/CC implication, because the late-time presence of large grains interior to the gap could be a remnant of the initial transient rather than ongoing leakage. The statement in Sec. 4.3 that 'the largest grains can still cross the gap intermittently' needs to be demonstrated independently of the pre-loaded population, for example by tracking the mass of grains that actually cross the gap after the gap is fully established.
minor comments (4)
  1. [Sec. 4.3 / Fig. 12] The text refers to 'panel [n]' for the 3 mm grains, but the panel labels in the figure are not alphabetically defined. Specify the exact panel.
  2. [Eq. (16)] The angle θ0 is defined earlier (Sec. 2.3) but would benefit from an explicit reminder here, since the piecewise definition uses θ0 and the expression cos^2(θ±θ0) is easy to misread.
  3. [Sec. 2.3] The cooling scheme is described as 'a quick β cool' which is ambiguous; clarify the notation and the relation to the locally isothermal limit.
  4. [Fig. 3 / footnote 3] The footnote correctly notes that the radial increase in transported mass partly reflects the larger mass reservoir at large radii. This caveat should be incorporated into the main text discussion of Fig. 3 to avoid over-interpreting the radial trend.

Circularity Check

0 steps flagged

No significant circularity: leaky-gap and size-filtering results are emergent simulation diagnostics, not fitted inputs or self-referential constructions.

full rationale

The paper's central claims are derived from its own simulation diagnostics rather than from fitted parameters or self-defining relations. The main evidence (integrated gas/dust mass crossing radius R in Figs. 3 and 12; face-on radial-flux maps in Figs. 4 and 13) is measured directly from the runs. The leaky-gap outcome is not forced by construction: in the 1 M_J case transport is initially suppressed and even reversed near ~12 au (Sec. 3.3: 'a pronounced suppression... net outward radial transport'), and only at late times do azimuthally intermittent inflow channels develop as the planet's torque becomes self-limiting and magnetic stresses reorganize into localized channels. The f(theta) atmospheric diffusivity boost (Eq. 16) is explicitly a modeling prescription 'to mimic the enhanced magnetic coupling... expected from increased ionization by stellar UV and X-ray irradiation,' inherited from Suriano et al. (2018); it is an untested but disclosed assumption affecting robustness, not a parameter fitted to the leaky-gap conclusion. Self-citations (Hsu et al. 2024, 2025; Hu et al. 2022, 2025) supply initial conditions, code lineage, and comparison checks; the planet-insertion results are new in this paper, and the same-group citations are corroborated by external works (Aoyama & Bai 2023; Wafflard-Fernandez & Lesur 2023). The paper explicitly credits independent hydro work for the incomplete-filtering concept (Sec. 5.2, citing Lubow & D'Angelo 2006, Bitsch et al. 2018, Huang et al. 2025, Homma et al. 2024), so it is not renaming a known result as novel. Its own flagged limitations (idealized planet insertion inflating 'pre-loading,' Sec. 5.2; reflective polar boundaries, Sec. 2.2; unresolved Hill-sphere capture, Sec. 5.3; no convergence study) are assumptions and scope caveats, not circular steps: the size-dependent filtration and intermittent channels emerge from the stated physics, and the acknowledged model-dependence of the wind strength is a vulnerability of the conclusion, not a logical identity between input and output.

Axiom & Free-Parameter Ledger

6 free parameters · 6 axioms · 1 invented entities

The 'leaky gap' conclusion rests on hand-chosen prescriptions: the f(theta) ionization enhancement that sustains the wind, the near-isothermal cooling, and the selected planet masses and dust bins. No constants were fitted to the target conclusions, and the setup is openly inherited from prior work. The main free parameters modulate the strength of the wind and thus the degree of leakage.

free parameters (6)
  • f(theta) diffusivity enhancement amplitude = exp(-cos^2(theta ± theta0) / (2(h/r)^2)) above/below disk
    Ad hoc boost of Ohmic and ambipolar diffusivities mimicking UV/X-ray ionization at disk surface. Directly controls wind strength and thus the persistence of leaky accretion channels; no independent constraint.
  • Cooling timescale = 10^-10 of local orbital period
    Effectively enforces locally isothermal behavior. Affects spiral shock dissipation and gap depth.
  • Planet masses = 0.01, 0.1, 1 MJ
    Three chosen sample points bracketing the regime transition; not fitted, but the conclusion about pebble isolation mass is extrapolated from one of these runs.
  • Dust grain sizes = five bins, 0.1 mm to 10 mm
    Chosen diagnostic bins following an MRN distribution; the size-dependent filtering result is expressed in terms of these bins.
  • Initial dust-to-gas ratio = epsilon = 0.01
    Standard assumption; affects dust feedback and drag coupling.
  • Midplane plasma beta = beta = 10^3
    Sets the initial poloidal field strength; inherited from prior work, but controls wind angular momentum transport.
axioms (6)
  • domain assumption Locally isothermal approximation via rapid cooling
    Section 2.1/2.3: the cooling timescale is 10^-10 of the orbital period, fixing the temperature profile. This suppresses thermal feedback that could alter gap structure.
  • domain assumption Pressureless dust fluid with linear drag law
    Eqs. (4)-(5) and dust module description: dust is a pressureless fluid coupled by a velocity-independent stopping time. Neglects dust diffusion and nonlinear drag, which can affect trapping efficiency.
  • domain assumption Fixed circular planet orbit, no migration or eccentricity
    Section 2.4 and footnote 1: the planet is placed on a fixed circular orbit; migration and eccentricity are excluded, although they can change substructure positions and gap permeability.
  • domain assumption Hydrostatic power-law initial disk, no initial radial velocity
    Section 2.3: density rho ∝ r^-1.5, T ∝ r^-1, vr=0. The transport results depend on the disk evolving from this state.
  • ad hoc to paper f(theta) ionization enhancement of diffusivities
    Section 2.5, Eq. (16): an ad hoc functional boost adopted from Suriano et al. (2018) to mimic stellar UV/X-ray irradiation. Its normalization is hand-chosen and is a load-bearing premise for wind-driven accretion.
  • domain assumption Simplified chemical network with MRN grain size distribution for non-ideal coefficients
    Section 2.5: diffusivities from Umebayashi & Nakano (1990)-style network with grains 0.5-25 microns; inherited from Hsu et al. (2024). Uncertainties in grain charge and ionization affect the dead-zone structure and wind strength.
invented entities (1)
  • none no independent evidence
    purpose: No new particles, fields, forces, or conserved quantities are introduced
    The paper introduces no novel entities; the 'azimuthally intermittent inflow channels' are emergent flow features, not new physics.

pith-pipeline@v1.3.0-alltime-deepseek · 24150 in / 11757 out tokens · 116048 ms · 2026-08-01T10:36:45.001520+00:00 · methodology

0 comments
read the original abstract

Radial dust transport in protoplanetary disks is a key process shaping planet formation and disk chemistry. We investigate how this transport, along with gas transport, is regulated in wind-launching disks with embedded planets using three-dimensional nonideal MHD simulations. We find that disk substructures do not act as absolute barriers to transport. Low-mass planets leave the disk structure dominated by the magnetic wind, while a Jupiter-mass planet opens a deep gap and drives spiral shocks. However, even in this regime, wind-driven accretion persists; the planet reshapes rather than replaces the magnetically driven flow, leaving the gap intrinsically time-dependent and partially permeable. Early-phase suppression of inward transport is followed by the development of localized, azimuthally intermittent inflow channels that enable continued cross-gap transport. This transport is strongly size-dependent: small grains remain coupled to the gas and readily penetrate the gap, whereas larger grains are efficiently trapped outside the planet. Consequently, a giant planet acts as an efficient but incomplete filter rather than a perfect barrier. These results support a "leaky gap" scenario, where radial transport is regulated rather than halted by substructures. Volatile-rich material can be delivered to the inner disk both before gap opening and via continued leakage, providing a natural explanation for the diverse inner disk compositions inferred from JWST. Similarly, pebble isolation during core growth should be viewed as a gradual filtering process rather than a binary transition. More generally, disk substructures are dynamically evolving features whose transport efficiency depends on their physical origin (magnetic versus planet-driven).

Figures

Figures reproduced from arXiv: 2607.20158 by Chun-Yen Hsu, Min-Kai Lin, Xiao Hu, Yisheng Tu, Zhi-Yun Li.

Figure 1
Figure 1. Figure 1: Gas surface density distributions at 𝑡 = 40 𝑇10 for disks hosting embedded planets of mass (a) 0.01 𝑀J , (b) 0.1 𝑀J , and (c) 1 𝑀J at (𝑟, 𝜃, 𝜙) = (10, 𝜋/2, 𝜋). The white dashed circles correspond to 𝑟 = 10 au. The lowest-mass planet produces only weak perturbations, leaving the wind-driven ring–gap structure largely intact. The intermediate-mass case exhibits a mixed morphology shaped by both magnetic stre… view at source ↗
Figure 2
Figure 2. Figure 2: The structures of the meridional plane slices centered at the azimuthal location of the embedded planet (𝜙 = 𝜋) for Model M001J, M01J, and M1J. Plotted in panels (a)-(c) are the gas density distribution (color map) and magnetic field lines (gray lines). Panels (d)-(f) show LIC (line integral convolution) streamlines for the poloidal gas motions. The dashed lines are isocurves of gas density, respectively 0… view at source ↗
Figure 3
Figure 3. Figure 3: Integrated gas mass (in units of Earth’s mass 𝑀⊕) crossing a given radius 𝑅 over successive 10 𝑇10 intervals for Models M001J (0.01 𝑀J , blue), M01J (0.1 𝑀J , black), and M1J (1 𝑀J , red). Positive values correspond to net inward transport. The vertical dashed line marks the planet’s orbit at 10 au. The integral is evaluated within two gas scale heights about the midplane. Wind-driven rings and gaps produc… view at source ↗
Figure 4
Figure 4. Figure 4: Panel (a) shows the face-on map of the vertically integrated radial gas mass flux for the 1 𝑀J model at 𝑡 = 40 𝑇10. Blue indicates inward radial transport and red outward radial transport. The white dashed circle corresponds to the planet orbit at 𝑟 = 10 au. Rather than forming an axisymmetric barrier, the outer gap region contains alternating azimuthal sectors of inward and outward radial transport associ… view at source ↗
Figure 5
Figure 5. Figure 5: Poloidal mass flux per unit area, 𝜌g𝑣pol, on a cone 8 angular scale heights above the midplane at 𝑡 = 40 𝑇10 for (a) the 1 𝑀J model and (b) the 0.01 𝑀J model. The color scale is logarithmic, with darker colors indicating lower mass flux. In the low-mass case, the wind-launching structure remains relatively smooth and nearly axisymmetric. In contrast, the Jupiter-mass planet produces a pronounced annular re… view at source ↗
Figure 6
Figure 6. Figure 6: Face-on surface density maps of the gas and different-sized dust grains in Model M001JD10mm01mm5bins at 𝑡 = 40𝑇10. All surface densities are normalized to their initial values and shown within a radius of 35 au. The white dashed circles correspond to 𝑟 = 10 au. The gas develops prominent ring–gap substructures produced by magnetic stresses in the wind-launching disk. Dust grains respond to these structures… view at source ↗
Figure 7
Figure 7. Figure 7: Azimuthally averaged radial surface density profiles of the gas and the five dust populations for Model M001JD10mm01mm5bins at 𝑡 = 40𝑇10, normalized to their initial values. The gas distribution exhibits moderate ra￾dial variations associated with magnetically generated rings and gaps. Small grains remain well coupled to the gas over most of the disk, whereas larger grains show strong concentration at smal… view at source ↗
Figure 8
Figure 8. Figure 8: Meridional slices at 𝜙 = 𝜋 (passing through the planet) for Model M001JD10mm01mm5bins illustrating the gas and dust dynamics. Panel (a) shows the gas density with magnetic field lines, while panel (b) displays the plasma-𝛽 distribution with gas velocity vectors. The thin high-𝛽 layer along the disk midplane marks the current sheet where both 𝐵𝑟 and 𝐵𝜙 reverse sign. Panels (c) and (d) show the dust-to-gas r… view at source ↗
Figure 9
Figure 9. Figure 9: Face-on surface density maps of the gas and different-sized dust grains in the 1 𝑀J planet model at 𝑡 = 40 𝑇10. All surface densities are normalized to their initial values and shown within a radius of 35 au. The white dashed circles correspond to 𝑟 = 10 au. The gas exhibits both magnetically generated ring–gap structures and spiral density waves launched by the planet. Dust responds to these structures in… view at source ↗
Figure 10
Figure 10. Figure 10: Azimuthally averaged radial surface density profiles of the gas and five dust populations in the 1 𝑀J model at 𝑡 = 40 𝑇10, normalized to their initial values. The gas surface density shows a deep planet-induced gap near 𝑅 ∼ 10 au together with surrounding ring–gap structures. Small grains remain well coupled to the gas and therefore broadly follow the gas distribution across most of the disk. Larger grain… view at source ↗
Figure 11
Figure 11. Figure 11: Meridional slices of the 1 𝑀J model at 𝑡 = 40 𝑇10 showing the gas density, plasma-𝛽, dust-to-gas ratio, and radial dust mass flux per unit area for representative grain sizes. The thin high-𝛽 layer along the midplane traces the magnetic current sheet where the horizontal magnetic field components reverse sign and where the fast midplane accretion stream is located. Compared with the lowest-mass (0.01 𝑀J) … view at source ↗
Figure 12
Figure 12. Figure 12: Integrated mass crossing a given radius 𝑅 over three time intervals (10–20, 20–30, and 30–40 𝑇10) for gas (in units of Earth’s mass) and dust grains of different sizes (in units of their initial mass within the disk in 𝑅 = 50 au). Rows correspond to gas and dust sizes of 10−1 , 10−0.5 , 100 , 100.5 , and 101 mm. Colors denote planet mass: 0.01 𝑀J (blue), 0.1 𝑀J (black), and 1 𝑀J (red). Positive values ind… view at source ↗
Figure 13
Figure 13. Figure 13: Face-on map of the vertically integrated radial mass flux of gas and dust in the 1 𝑀J model at 𝑡 = 40 𝑇10. Blue indicates inward radial transport and red outward radial transport. The thick white solid circles correspond to the planet orbit at 𝑟 = 10 au. The thinner white dashed circles correspond to the 𝑟 = 5, 8, 12, 15, and 20 au. The instantaneous transport pattern is highly non-axisymmetric, consistin… view at source ↗
Figure 14
Figure 14. Figure 14: Gas and dust spatial distributions near the CPD at 𝑡 = 40 𝑇10. Panel (a) shows the gas surface density normalized by its initial (unperturbed) value, highlighting the dense CPD within the planet’s Hill sphere. Panels (b)–(f) show the dust-to-gas surface density ratio for each of the five dust bins, normalized to their initial values. The purple and green circular lines correspond to the planet’s Hill Sphe… view at source ↗

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Works this paper leans on

180 extracted references · 12 canonical work pages · 6 internal anchors

  1. [1]

    , keywords =

    Rapid growth of gas-giant cores by pebble accretion. , keywords =. doi:10.1051/0004-6361/201219127 , archivePrefix =. 1205.3030 , primaryClass =

    Pith/arXiv arXiv

  2. [2]

    , keywords =

    Forming the cores of giant planets from the radial pebble flux in protoplanetary discs. , keywords =. doi:10.1051/0004-6361/201424343 , archivePrefix =. 1408.6094 , primaryClass =

    Pith/arXiv arXiv

  3. [3]

    Lubow, S. H. and D'Angelo, G. , title =. The Astrophysical Journal , year =

  4. [4]

    and Lambrechts, M

    Bitsch, B. and Lambrechts, M. and Johansen, A. , title =. Astronomy & Astrophysics , year =

  5. [5]

    and Dong, Ruobing and Bai, Xue-Ning , title =

    Huang, Pinghui and Yu, Fangyuan and Lee, Eve J. and Dong, Ruobing and Bai, Xue-Ning , title =. The Astrophysical Journal , year =

  6. [6]

    2014 , volume =

    Forming the cores of giant planets from the radial pebble flux in protoplanetary disks , journal =. 2014 , volume =

    2014

  7. [7]

    2019 , volume =

    Formation of giant planet cores by pebble accretion , journal =. 2019 , volume =

    2019

  8. [8]

    2017 , volume =

    Age of Jupiter inferred from the distinct genetics and formation times of meteorites , journal =. 2017 , volume =

    2017

  9. [9]

    2020 , volume =

    Constraining the formation of Jupiter through meteorite chronology , journal =. 2020 , volume =

    2020

  10. [10]

    2011 , volume =

    Stable-isotopic anomalies and the accretionary assemblage of the Earth and Mars , journal =. 2011 , volume =

    2011

  11. [11]

    2020 , volume =

    The partitioning of the inner and outer Solar System by a structured protoplanetary disk , journal =. 2020 , volume =

    2020

  12. [12]

    2023 , volume =

    JWST Reveals Cool Water Reservoirs in Protoplanetary Disks , journal =. 2023 , volume =

    2023

  13. [13]

    2025 , note =

    MINDS: Linking Outer Disk Substructures to Inner Disk Chemistry , journal =. 2025 , note =

    2025

  14. [14]

    2025 , volume =

    JDISC: Molecular Emission from Inner Protoplanetary Disks with JWST , journal =. 2025 , volume =

    2025

  15. [15]

    2025 , volume =

    JWST Observations of GM Aur: Molecular Depletion in a Disk Cavity , journal =. 2025 , volume =

    2025

  16. [16]

    2023 , volume =

    Water Vapor in the Terrestrial Zone of the PDS 70 Disk , journal =. 2023 , volume =

    2023

  17. [17]

    , year = 2002, month = apr, volume =

    Nonlinear Propagation of Planet-generated Density Waves and Gap Opening Criterion in Protoplanetary Disks. , year = 2002, month = apr, volume =. doi:10.1086/339471 , adsurl =

    doi:10.1086/339471 2002

  18. [18]

    , year = 2006, month = jul, volume =

    Hydraulic/Shock Bores in Protoplanetary Disks. , year = 2006, month = jul, volume =. doi:10.1086/500445 , adsurl =

    work page doi:10.1086/500445 2006

  19. [19]

    , year = 2016, month = dec, volume =

    How Empty Are Disk Gaps Opened by Giant Planets?. , year = 2016, month = dec, volume =. doi:10.3847/0004-637X/832/2/105 , adsurl =

    doi:10.3847/0004-637x/832/2/105 2016

  20. [20]

    , keywords =

    Rossby Wave Instability in Locally Isothermal and Polytropic Disks: Three-dimensional Linear Calculations. , keywords =. doi:10.1088/0004-637X/754/1/21 , archivePrefix =. 1203.2630 , primaryClass =

    Pith/arXiv arXiv

  21. [21]

    Protostars and Planets VII , year = 2023, editor =

    Structured Distributions of Gas and Solids in Protoplanetary Disks. Protostars and Planets VII , year = 2023, editor =. doi:10.48550/arXiv.2210.13314 , archivePrefix =. 2210.13314 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.2210.13314 2023

  22. [22]

    , keywords =

    Formation of dust rings and gaps in non-ideal MHD discs through meridional gas flows. , keywords =. doi:10.1093/mnras/stac1799 , archivePrefix =. 2203.05629 , primaryClass =

    arXiv

  23. [23]

    , keywords =

    Mechanism of Magnetic Flux Loss in Molecular Clouds. , keywords =. doi:10.1086/340587 , archivePrefix =. astro-ph/0203223 , primaryClass =

    Pith/arXiv arXiv

  24. [24]

    , keywords =

    Magnetic flux loss from interstellar clouds. , keywords =. doi:10.1093/mnras/243.1.103 , adsurl =

    work page doi:10.1093/mnras/243.1.103

  25. [25]

    I - Formulation and conditions for efficient dissipation

    Dissipation of magnetic fields in very dense interstellar clouds. I - Formulation and conditions for efficient dissipation. , keywords =. doi:10.1093/mnras/218.4.663 , adsurl =

    work page doi:10.1093/mnras/218.4.663

  26. [26]

    , keywords =

    Magnetic Flux Loss from Interstellar Clouds with Various Grain-Size Distributions. , keywords =. doi:10.1086/169682 , adsurl =

    work page doi:10.1086/169682

  27. [27]

    , keywords =

    On the importance of disc chemistry in the formation of protoplanetary disc rings. , keywords =. doi:10.1093/mnras/stad2626 , archivePrefix =. 2308.12946 , primaryClass =

    Pith/arXiv arXiv

  28. [28]

    , keywords =

    Effect of grain size on differential desorption of volatile species and on non-ideal MHD diffusivity. , keywords =. doi:10.1093/mnras/sty1165 , archivePrefix =. 1803.03062 , primaryClass =

    Pith/arXiv arXiv

  29. [29]

    , keywords =

    The challenges of modelling microphysics: ambipolar diffusion, chemistry, and cosmic rays in MHD shocks. , keywords =. doi:10.1093/mnras/sty3519 , archivePrefix =. 1901.00504 , primaryClass =

    Pith/arXiv arXiv 1901

  30. [30]

    , keywords =

    Magneto-thermal Disk Winds from Protoplanetary Disks. , keywords =. doi:10.3847/0004-637X/818/2/152 , archivePrefix =. 1511.06769 , primaryClass =

    Pith/arXiv arXiv

  31. [31]

    , keywords =

    Hall Effect-Mediated Magnetic Flux Transport in Protoplanetary Disks. , keywords =. doi:10.3847/1538-4357/836/1/46 , archivePrefix =. 1612.03912 , primaryClass =

    Pith/arXiv arXiv

  32. [32]

    , keywords =

    A Fast and Accurate Calculation Scheme for Ionization Degrees in Protoplanetary and Circumplanetary Disks with Charged Dust Grains. , keywords =. doi:10.1088/0004-637X/743/1/53 , archivePrefix =. 1106.3528 , primaryClass =

    Pith/arXiv arXiv

  33. [33]

    , keywords =

    The UMIST database for astrochemistry 2012. , keywords =. doi:10.1051/0004-6361/201220465 , archivePrefix =. 1212.6362 , primaryClass =

    Pith/arXiv arXiv 2012

  34. [34]

    , keywords =

    The size distribution of interstellar grains. , keywords =. doi:10.1086/155591 , adsurl =

    doi:10.1086/155591

  35. [35]

    , keywords =

    Collisional Charging of Interstellar Grains. , keywords =. doi:10.1086/165596 , adsurl =

    doi:10.1086/165596

  36. [36]

    , keywords =

    Magnetorotational-instability-driven Accretion in Protoplanetary Disks. , keywords =. doi:10.1088/0004-637X/739/1/50 , archivePrefix =. 1107.2935 , primaryClass =

    Pith/arXiv arXiv

  37. [37]

    Saas-Fee Advanced Course , keywords =

    Physical Processes in Protoplanetary Disks. Saas-Fee Advanced Course , keywords =. doi:10.1007/978-3-662-58687-7_1 , adsurl =

    doi:10.1007/978-3-662-58687-7_1

  38. [38]

    Three-fluid plasmas in star formation. I. Magneto-hydrodynamic equations. , keywords =. doi:10.1051/0004-6361:20078818 , archivePrefix =. 0804.2826 , primaryClass =

    Pith/arXiv arXiv

  39. [39]

    , keywords =

    Magnetic fields in protoplanetary disks. , keywords =. doi:10.1007/s10509-007-9575-8 , archivePrefix =. 0704.0970 , primaryClass =

    Pith/arXiv arXiv

  40. [40]

    Physics of Plasmas , keywords =

    Radiation pressure and gas drag forces on a melamine-formaldehyde microsphere in a dusty plasma. Physics of Plasmas , keywords =. doi:10.1063/1.1526701 , adsurl =

    doi:10.1063/1.1526701

  41. [41]

    , keywords =

    The formation of rings and gaps in magnetically coupled disc-wind systems: ambipolar diffusion and reconnection. , keywords =. doi:10.1093/mnras/sty717 , archivePrefix =. 1712.06217 , primaryClass =

    Pith/arXiv arXiv

  42. [42]

    , keywords =

    Linear and non-linear evolution of the vertical shear instability in accretion discs. , keywords =. doi:10.1093/mnras/stt1475 , archivePrefix =. 1209.2753 , primaryClass =

    Pith/arXiv arXiv

  43. [43]

    The effects of disk resistivity

    MHD simulations of jet acceleration from Keplerian accretion disks. The effects of disk resistivity. , keywords =. doi:10.1051/0004-6361:20066400 , archivePrefix =. astro-ph/0703064 , primaryClass =

    Pith/arXiv arXiv

  44. [44]

    , keywords =

    The Structure of Spiral Shocks Excited by Planetary-mass Companions. , keywords =. doi:10.1088/0004-637X/813/2/88 , archivePrefix =. 1507.03599 , primaryClass =

    Pith/arXiv arXiv

  45. [45]

    , keywords =

    Global Evolution of an Accretion Disk with a Net Vertical Field: Coronal Accretion, Flux Transport, and Disk Winds. , keywords =. doi:10.3847/1538-4357/aaafc9 , archivePrefix =. 1701.04627 , primaryClass =

    Pith/arXiv arXiv

  46. [46]

    , keywords =

    Disc formation in magnetized dense cores with turbulence and ambipolar diffusion. , keywords =. doi:10.1093/mnras/stz2436 , archivePrefix =. 1908.11806 , primaryClass =

    Pith/arXiv arXiv 1908

  47. [47]

    Physics of Astrophysics, Vol. II

  48. [48]

    Turbulence and dust-gas dynamics at non-linear saturation

    Streaming instability with multiple dust species - II. Turbulence and dust-gas dynamics at non-linear saturation. , keywords =. doi:10.1093/mnras/stab2959 , archivePrefix =. 2110.06248 , primaryClass =

    Pith/arXiv arXiv

  49. [49]

    , keywords =

    Global three-dimensional simulations of outer protoplanetary discs with ambipolar diffusion. , keywords =. doi:10.1093/mnras/stab2220 , archivePrefix =. 2106.10167 , primaryClass =

    Pith/arXiv arXiv

  50. [50]

    , keywords =

    Streaming Instabilities in Protoplanetary Disks. , keywords =. doi:10.1086/426895 , archivePrefix =. astro-ph/0409263 , primaryClass =

    Pith/arXiv arXiv

  51. [51]

    , keywords =

    Nonlinear Evolution of Streaming Instabilities in Accreting Protoplanetary Disks. , keywords =. doi:10.3847/1538-4357/ac8df9 , archivePrefix =. 2209.06784 , primaryClass =

    Pith/arXiv arXiv

  52. [52]

    , keywords =

    Nonlocal stability analysis of the MHD Kelvin-Helmholtz instability in a compressible plasma. , keywords =. doi:10.1029/JA087iA09p07431 , adsurl =

    work page doi:10.1029/ja087ia09p07431

  53. [53]

    , keywords =

    The 2014 ALMA Long Baseline Campaign: First Results from High Angular Resolution Observations toward the HL Tau Region. , keywords =. doi:10.1088/2041-8205/808/1/L3 , archivePrefix =. 1503.02649 , primaryClass =

    Pith/arXiv arXiv 2014

  54. [54]

    The Disk Substructures at High Angular Resolution Project (DSHARP). I. Motivation, Sample, Calibration, and Overview. , keywords =. doi:10.3847/2041-8213/aaf741 , archivePrefix =. 1812.04040 , primaryClass =

    Pith/arXiv arXiv 2041

  55. [55]

    , keywords =

    The formation of rings and gaps in wind-launching non-ideal MHD discs: three-dimensional simulations. , keywords =. doi:10.1093/mnras/sty3502 , archivePrefix =. 1810.02234 , primaryClass =

    Pith/arXiv arXiv

  56. [56]

    , year = 1978, month = dec, volume =

    Review of Publications: Physical Processes in the Interstellar Medium. , year = 1978, month = dec, volume =

    1978

  57. [57]

    , keywords =

    The Athena++ Adaptive Mesh Refinement Framework: Design and Magnetohydrodynamic Solvers. , keywords =. doi:10.3847/1538-4365/ab929b , archivePrefix =. 2005.06651 , primaryClass =

    Pith/arXiv arXiv 2005

  58. [58]

    , keywords =

    Thresholds for Particle Clumping by the Streaming Instability. , keywords =. doi:10.3847/1538-4357/ac0e9f , archivePrefix =. 2105.06042 , primaryClass =

    Pith/arXiv arXiv

  59. [59]

    , keywords =

    Rossby wave instability does not require sharp resistivity gradients. , keywords =. doi:10.1051/0004-6361/201424919 , archivePrefix =. 1410.8092 , primaryClass =

    Pith/arXiv arXiv

  60. [60]

    Rossby Wave Instability of Thin Accretion Disks. II. Detailed Linear Theory. , keywords =. doi:10.1086/308693 , archivePrefix =. astro-ph/9907279 , primaryClass =

    Pith/arXiv arXiv

  61. [61]

    , keywords =

    Impact of local pressure enhancements on dust concentration in turbulent protoplanetary discs. , keywords =. doi:10.1051/0004-6361/202142378 , archivePrefix =. 2112.06153 , primaryClass =

    Pith/arXiv arXiv

  62. [62]

    , keywords =

    Rossby Wave Instability of Keplerian Accretion Disks. , keywords =. doi:10.1086/306900 , archivePrefix =. astro-ph/9809321 , primaryClass =

    Pith/arXiv arXiv

  63. [63]

    , keywords =

    Parametric Study of the Rossby Wave Instability in a Two-dimensional Barotropic Disk. , keywords =. doi:10.3847/0004-637X/823/2/84 , archivePrefix =. 1603.09225 , primaryClass =

    Pith/arXiv arXiv

  64. [64]

    , keywords =

    Structure Formation in a Young Protoplanetary Disk by a Magnetic Disk Wind. , keywords =. doi:10.3847/1538-4357/aadda0 , archivePrefix =. 1808.10220 , primaryClass =

    Pith/arXiv arXiv

  65. [65]

    Wind-driven Accretion in Protoplanetary Disks. I. Suppression of the Magnetorotational Instability and Launching of the Magnetocentrifugal Wind. , keywords =. doi:10.1088/0004-637X/769/1/76 , archivePrefix =. 1301.0318 , primaryClass =

    Pith/arXiv arXiv

  66. [66]

    , keywords =

    Systematic description of wind-driven protoplanetary discs. , keywords =. doi:10.1051/0004-6361/202040109 , archivePrefix =. 2101.10349 , primaryClass =

    Pith/arXiv arXiv

  67. [67]

    Physical Review , year = 1924, month = jun, volume =

    On the Resistance Experienced by Spheres in their Motion through Gases. Physical Review , year = 1924, month = jun, volume =. doi:10.1103/PhysRev.23.710 , adsurl =

    doi:10.1103/physrev.23.710 1924

  68. [68]

    arXiv e-prints , keywords =

    Physical processes in protoplanetary disks. arXiv e-prints , keywords =. doi:10.48550/arXiv.1509.06382 , archivePrefix =. 1509.06382 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.1509.06382

  69. [69]

    , keywords =

    Protoplanetary Disk Rings as Sites for Planetesimal Formation. , keywords =. doi:10.3847/1538-3881/abd4d9 , archivePrefix =. 2008.01727 , primaryClass =

    Pith/arXiv arXiv 2008

  70. [70]

    , keywords =

    Emergence of vortices at the edges of planet-driven gaps in protoplanetary discs. , keywords =. doi:10.1093/mnras/stac3507 , archivePrefix =. 2212.03062 , primaryClass =

    Pith/arXiv arXiv

  71. [71]

    , keywords =

    Vortex-like kinematic signal, spirals, and beam smearing effect in the HD 142527 disk. , keywords =. doi:10.1051/0004-6361/202040089 , archivePrefix =. 2103.13474 , primaryClass =

    Pith/arXiv arXiv

  72. [72]

    Gaps Opened by Single and Multiple Young Planets in Disks

    Observational Signatures of Planets in Protoplanetary Disks I. Gaps Opened by Single and Multiple Young Planets in Disks. , keywords =. doi:10.1088/0004-637X/809/1/93 , archivePrefix =. 1411.6063 , primaryClass =

    Pith/arXiv arXiv

  73. [73]

    , keywords =

    On the Formation of Multiple Concentric Rings and Gaps in Protoplanetary Disks. , keywords =. doi:10.3847/1538-4357/aa9705 , archivePrefix =. 1706.03066 , primaryClass =

    Pith/arXiv arXiv

  74. [74]

    , keywords =

    Sintering-induced Dust Ring Formation in Protoplanetary Disks: Application to the HL Tau Disk. , keywords =. doi:10.3847/0004-637X/821/2/82 , archivePrefix =. 1510.03556 , primaryClass =

    Pith/arXiv arXiv

  75. [75]

    From simulations to ALMA observations

    Gaps, rings, and non-axisymmetric structures in protoplanetary disks. From simulations to ALMA observations. , keywords =. doi:10.1051/0004-6361/201424693 , archivePrefix =. 1411.2736 , primaryClass =

    Pith/arXiv arXiv

  76. [76]

    , keywords =

    Gaps, rings, and non-axisymmetric structures in protoplanetary disks: Emission from large grains. , keywords =. doi:10.1051/0004-6361/201526616 , archivePrefix =. 1603.05179 , primaryClass =

    Pith/arXiv arXiv

  77. [77]

    , keywords =

    Zonal Flows and Long-lived Axisymmetric Pressure Bumps in Magnetorotational Turbulence. , keywords =. doi:10.1088/0004-637X/697/2/1269 , archivePrefix =. 0811.3937 , primaryClass =

    Pith/arXiv arXiv

  78. [78]

    , keywords =

    Dust Segregation in Hall-dominated Turbulent Protoplanetary Disks. , keywords =. doi:10.3847/1538-4357/aadcf0 , archivePrefix =. 1808.07660 , primaryClass =

    Pith/arXiv arXiv

  79. [79]

    Axisymmetric resistive MHD simulations

    Rings and gaps produced by variable magnetic disc winds and avalanche accretion streams - I. Axisymmetric resistive MHD simulations. , keywords =. doi:10.1093/mnras/stx735 , archivePrefix =. 1702.01565 , primaryClass =

    Pith/arXiv arXiv

  80. [80]

    , keywords =

    Spontaneous ring formation in wind-emitting accretion discs. , keywords =. doi:10.1051/0004-6361/201834813 , archivePrefix =. 1904.07910 , primaryClass =

    Pith/arXiv arXiv 1904

Showing first 80 references.