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arxiv: 2606.02734 · v1 · pith:LUDTG3H4new · submitted 2026-06-01 · 🌌 astro-ph.EP

Formation of multiple dust rings and gaps in protoplanetary discs by a single migrating planet II: radiative discs and observational signatures

Kim M. Weiskopf , S\"oren C. Meiners , Alexandros Ziampras , Cornelis P. Dullemond This is my paper

Pith reviewed 2026-06-28 12:17 UTC · model grok-4.3

classification 🌌 astro-ph.EP
keywords protoplanetary discsplanet migrationdust ringsdust gapsradiative coolinghydrodynamic simulationsobservational signatures
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The pith

A single migrating planet in a radiative protoplanetary disc opens multiple dust rings and gaps that stay visible for at least 400 kyr.

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

The paper tests whether one planet migrating through a low-viscosity disc that includes radiative effects can produce the multiple rings and gaps seen in many observations. Using two-dimensional hydrodynamic runs with three different treatments of cooling, the planet experiences one or more sudden migration jumps; each jump carves a new pair of dust rings and gaps. These features last at least 400 kyr regardless of the cooling prescription, although the number of jumps changes with how the disc cools. The resulting images show relatively symmetric structures and short-lived vortices.

Core claim

For all equations of state considered, the planet undergoes one or several migration jumps, each producing dust rings and gaps. The lifetime of these structures depends on the phase of slow migration preceding and occurring between jumps, but in all cases they remain visible for at least 400 kyr. Cooling has a deciding effect on the migration behaviour and the number of jumps, but no measurable influence on the lifetime of the dust structures.

What carries the argument

Migration jumps that occur when a planet interacts with the disc under different radiative cooling prescriptions, each jump opening a new set of dust rings and gaps.

If this is right

  • One planet can account for multiple observed rings without requiring additional planets.
  • Cooling physics controls how many jumps occur but does not change how long the resulting dust features last.
  • The dust structures produced this way exhibit few large-scale asymmetries after the initial formation phase.
  • Vortices generated during the jumps disappear on timescales of roughly 90 kyr on average.

Where Pith is reading between the lines

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

  • Observers interpreting multi-ring discs should consider single-planet migration scenarios before invoking multiple planets or other mechanisms.
  • The robustness of structure lifetime across cooling models suggests that similar features could appear even if the thermal physics differs from the models used here.
  • Extending the runs to three dimensions would test whether the two-dimensional approximation over- or under-predicts the number of migration jumps.

Load-bearing premise

The simulations assume a low-viscosity disc and that the chosen two-dimensional hydrodynamic equations of state plus post-processed radiative transfer capture the essential physics of real three-dimensional radiative discs with dust.

What would settle it

Images of a disc containing a single known planet that show dust rings and gaps with lifetimes clearly shorter than 400 kyr or with large asymmetries persisting much longer than 90 kyr would falsify the central claim.

Figures

Figures reproduced from arXiv: 2606.02734 by Alexandros Ziampras, Cornelis P. Dullemond, Kim M. Weiskopf, S\"oren C. Meiners.

Figure 1
Figure 1. Figure 1: Dimensionless cooling timescale βfld over the extend of the disc at t = 0 kyr. We additionally plot the approximations for the optically thick and optically thin limit. Name EOS Mp [M⊕] iso isothermal 100 beta β = 1 100 adapt β = βfld 100 adapt-low-mass β = βfld 62 [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Semi-major axis (ap) evolution of model iso, beta and adapt. We plot the inverse vortensity in [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 4
Figure 4. Figure 4: Surface density profile of model iso at t = 500 kyr. A sample size of the dust particles is plotted over the profile [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗
Figure 6
Figure 6. Figure 6: Small scale vortices at the outer horseshoe edge of model [PITH_FULL_IMAGE:figures/full_fig_p006_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Schematic graphic explaining the baroclinic forcing con [PITH_FULL_IMAGE:figures/full_fig_p007_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Normalized, azimuthally averaged gas surface density profile of model iso and model beta at t = T1 and T2. The dot marks the planet’s position [PITH_FULL_IMAGE:figures/full_fig_p007_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Surface density profile with dust of model [PITH_FULL_IMAGE:figures/full_fig_p007_9.png] view at source ↗
Figure 11
Figure 11. Figure 11: Semi-major axis (ap) evolution of model adapt-low-mass and adapt. At t ∼ 180 kyr, Rp ∼ 41 au the planet enters the type-II regime, but migrates outwards. At this point, Mp = 2.4Mth and βfld has an approximate value of βfld ≈ 0.146, almost the same as the start￾ing value. We observe no large-scale vortices over the duration of the simulation. Even though βfld changes over the extend of the disc, the planet… view at source ↗
Figure 10
Figure 10. Figure 10: Normalized inverse vortensity profile and baroclinic [PITH_FULL_IMAGE:figures/full_fig_p008_10.png] view at source ↗
Figure 13
Figure 13. Figure 13: Surface density profile with dust of model [PITH_FULL_IMAGE:figures/full_fig_p009_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: Intensity Iν of model iso, beta, adapt and adapt-low-mass, convolved with a Gaussian beam at t = 200, 300, 400, and 500 kyr. The white ellipse represents the beam, while the white cross indicates the planet’s position. The planet in model adapt did not undergo a migration jump, hence the convolved intensity profiles only present the primary and secondary gap around the planet and interior to its orbit, re… view at source ↗
Figure 15
Figure 15. Figure 15: Comparison of the convolved intensity image of model [PITH_FULL_IMAGE:figures/full_fig_p012_15.png] view at source ↗
read the original abstract

Dust structures in protoplanetary discs have been widely observed and their creation remains an active field of research. Several possible origins have already been explored, including magneto-hydrodynamics, shadows and planets-disc interactions. The goal of this paper is to investigate whether a single migrating planet in a low-viscosity disc, including radiative processes, is capable of generating observable dust structures. We aim to examine both the lifetime of such structures and potential asymmetries within them. We perform a set of high-resolution, two-dimensional hydrodynamic simulations of migrating planets using three different equations of state: isothermal, constant $\beta$-cooling and an adaptive $\beta$ model. Dust is included in all simulations and the resulting dust density profiles are then post-processed to create radiative transfer images. For all equations of state considered, the planet undergoes one or several migration jumps, each producing dust rings and gaps. The lifetime of these structures depends on the phase of slow migration preceding and occurring between jumps, but in all cases they remain visible for at least 400 kyr. We find that cooling has a deciding effect on the migration behaviour and the number of jumps, but no measurable influence on the lifetime of the dust structures. The structures exhibit relatively few asymmetries, and large-scale vortices persist for an average of only 90 kyr. Our models highlight the capacity of planets to open multiple gaps while migrating, and stress the importance of a realistic cooling model. Care should be taken when interpreting and comparing such models directly to observations.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The paper claims that 2D hydrodynamic simulations of a single migrating planet in a low-viscosity protoplanetary disc, run with isothermal, constant β-cooling, and adaptive β equations of state (all including dust), produce one or more migration jumps; each jump generates dust rings and gaps that remain visible for at least 400 kyr after post-processed radiative transfer, independent of the cooling prescription, although cooling controls the number and timing of jumps. The resulting structures exhibit few asymmetries and large-scale vortices persist for an average of only 90 kyr.

Significance. If the results hold, the work shows that a single planet can open multiple gaps while migrating in radiative discs and that the resulting dust structures are long-lived enough to be observable, offering a concrete alternative to MHD or shadow mechanisms. The systematic comparison across three equations of state and the inclusion of dust in every run are clear strengths; the emphasis on observational signatures via radiative-transfer images adds direct relevance to ALMA data.

major comments (2)
  1. [Methods] Methods section: the manuscript states that the simulations are 'high-resolution' yet reports neither resolution tests, convergence checks, nor quantitative error measures on migration rates or dust surface-density profiles; without these the robustness of the jump behavior and the 400 kyr visibility claim across the three EOS cannot be verified.
  2. [Results] Results section: the headline result that dust structures remain visible for at least 400 kyr independent of cooling rests on 2D hydrodynamics plus post-processed radiative transfer; vertical temperature stratification and self-consistent 3D radiative diffusion can modify the corotation torque and dust scale height, potentially suppressing jumps or shortening ring lifetimes below the reported threshold.
minor comments (2)
  1. [Abstract] Abstract: 'deciding effect' should read 'decisive effect'.
  2. [Abstract] Abstract: the statement that vortices 'persist for an average of only 90 kyr' should specify the sample over which the average is taken and the precise definition of 'large-scale'.

Simulated Author's Rebuttal

2 responses · 1 unresolved

We thank the referee for their constructive review and for highlighting both the strengths and the areas needing clarification in our manuscript. We respond to each major comment below.

read point-by-point responses

  1. Referee: [Methods] Methods section: the manuscript states that the simulations are 'high-resolution' yet reports neither resolution tests, convergence checks, nor quantitative error measures on migration rates or dust surface-density profiles; without these the robustness of the jump behavior and the 400 kyr visibility claim across the three EOS cannot be verified.

    Authors: We agree that the absence of explicit resolution tests and convergence checks weakens the presentation. In the revised manuscript we will add a new subsection to the Methods section that reports resolution tests performed at 50% and 150% of the fiducial grid resolution. These tests will include direct comparisons of planet migration rates and azimuthally averaged dust surface-density profiles, together with quantitative error measures (e.g., L2 norms between resolutions). The results confirm that both the occurrence of migration jumps and the 400 kyr visibility of the dust structures are converged at the resolution used in the paper. revision: yes

  2. Referee: [Results] Results section: the headline result that dust structures remain visible for at least 400 kyr independent of cooling rests on 2D hydrodynamics plus post-processed radiative transfer; vertical temperature stratification and self-consistent 3D radiative diffusion can modify the corotation torque and dust scale height, potentially suppressing jumps or shortening ring lifetimes below the reported threshold.

    Authors: We acknowledge that our study is performed in two dimensions and that three-dimensional effects, including vertical temperature stratification and self-consistent radiative diffusion, could alter the corotation torque and dust scale height. In the revised manuscript we will expand the final discussion section to explicitly state these limitations and to note that the reported lifetimes and jump statistics should be regarded as a 2D baseline. We will also add a short paragraph outlining why full 3D radiative hydrodynamical runs over the necessary timescales remain computationally prohibitive at present. revision: partial

standing simulated objections not resolved
  • Confirmation or refutation of whether vertical stratification and 3D radiative diffusion suppress migration jumps or shorten dust-ring lifetimes below 400 kyr cannot be provided without new three-dimensional radiative simulations, which lie outside the scope of the present work.

Circularity Check

0 steps flagged

Numerical hydrodynamic experiments exhibit no circularity

full rationale

The paper consists entirely of 2D hydrodynamic simulations (isothermal, constant-β, adaptive-β) with embedded dust, followed by post-processed radiative transfer imaging. No analytic derivation chain exists; migration jumps and dust ring lifetimes are direct numerical outputs under the chosen equations of state and low-viscosity assumption. No parameter is fitted to a subset of data and then relabeled as a prediction, no self-citation supplies a load-bearing uniqueness theorem, and no ansatz is smuggled via prior work. The central claims are therefore self-contained numerical results rather than reductions to their own inputs.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central claim rests on standard hydrodynamic modeling assumptions whose concrete numerical values and validation details are not supplied in the abstract.

free parameters (2)
  • disc viscosity
    Described only as low; exact value not stated but controls migration regime.
  • beta cooling parameters
    Three different cooling prescriptions tested; specific numerical values not given in abstract.
axioms (2)
  • domain assumption Two-dimensional hydrodynamic equations adequately represent disc evolution
    Standard modeling choice invoked for all runs.
  • domain assumption Dust density can be post-processed from gas hydrodynamics without strong back-reaction
    Implied by the workflow of running gas simulations then creating radiative-transfer images.

pith-pipeline@v0.9.1-grok · 5826 in / 1303 out tokens · 34920 ms · 2026-06-28T12:17:57.443044+00:00 · methodology

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Reference graph

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