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Planet formation at the inner edge of the dead zone II. Outbursts, rings, vortices, and suppression of planetesimal formation

T0 review · 2 major / 1 minor · reviewed 2026-06-27 · grok-4.3

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Pith's one-line read Accretion outbursts trigger vortices that suppress planetesimal formation in protoplanetary disks

desk verdict 2D simulations show outbursts spawning vortices that suppress planetesimals via diffusion, but the vertical integration leaves 3D robustness untested. read the letter →

arxiv 2606.11344 v1 pith:S7KJOZUO submitted 2026-06-09 astro-ph.EP

Alexandros Ziampras , Tilman Birnstiel This is my paper · ORCID
classification astro-ph.EP
keywords accretionoutburstsRossbywaveinstabilityvorticesplanetesimalformationprotoplanetarydisksplanetdeadzoneturbulentdiffusion
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 examines how accretion outbursts behave in the inner regions of protoplanetary disks using detailed 2D simulations that include radiation and dust growth. The simulations reveal that these outbursts break apart due to an instability, forming multiple small vortices that merge into a single large one over time. These vortices create strong mixing that prevents dust particles from accumulating into planetesimals. The findings indicate that such events are likely to disrupt planet formation temporarily, but the disk settles back into a stable configuration afterward where formation can resume.

What carries the argument

Rossby-wave instability applied to the accretion outburst front in multifluid radiation-hydrodynamical simulations, leading to vortex formation and turbulent diffusion

What would settle it

Observing an accretion outburst without the formation of vortices or with ongoing planetesimal formation during the burst would contradict the findings

Watch

Extended reading notes

Core claim

Accretion outbursts are highly unstable to the Rossby-wave instability, with the burst front quickly diffusing into a large number of small-scale vortices that coalesce over time into a single, compact vortex and inducing azimuthal asymmetries. Vortices act as a source of vigorous turbulent diffusion, strongly suppressing planetesimal formation. Our results suggest that azimuthal asymmetries associated with accretion outbursts should be both common and detrimental to planet formation. Nevertheless, planetesimal formation will resume post-burst, as the burst-induced vortices eventually decay and the disk returns to a quiescent state featuring a pressure bump at ~1 au.

Load-bearing premise

The two-dimensional vertically integrated simulation setup with growing dust and radiation transport accurately represents the stability and dust behavior in actual three-dimensional disks

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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

2 major / 1 minor

Summary. The manuscript uses high-resolution 2D vertically integrated multifluid radiation-hydrodynamical simulations of the inner 10 au of protoplanetary disks with dynamically growing dust and realistic opacity to study accretion outbursts. It claims that outbursts are highly unstable to the Rossby-wave instability, with the burst front diffusing into small-scale vortices that coalesce into a single compact vortex, inducing azimuthal asymmetries; these vortices drive vigorous turbulent diffusion that strongly suppresses planetesimal formation, although formation resumes post-burst once vortices decay and a pressure bump reforms at ~1 au.

Significance. If the central results hold, the work identifies a mechanism linking observed accretion outbursts to common azimuthal asymmetries that hinder planetesimal formation during the burst phase. The multifluid treatment with radiation transport and realistic dust opacity provides a more complete dynamical picture than prior axisymmetric models.

major comments (2)
  1. [Methods] Methods section (and abstract): The headline claims on RWI-driven vortex formation and strong suppression of planetesimal formation rest exclusively on the 2D vertically integrated equations; no 3D control runs or explicit justification is provided that vertical shear, buoyancy frequency, and dust sedimentation are adequately captured for linear growth rates and nonlinear vortex lifetime, which is load-bearing for the central claim.
  2. [Results] Results (vortex diffusion and planetesimal suppression): The quantitative assertion that vortices 'strongly suppress' planetesimal formation via turbulent diffusion lacks reported convergence tests, resolution studies, or error analysis on the dust growth implementation, making the strength of the suppression difficult to evaluate independently.
minor comments (1)
  1. [Abstract] Abstract: The phrase 'high-resolution' is used without stating the grid resolution or cell count, which would improve reproducibility and clarity.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed comments on our manuscript. We address each major comment point by point below and outline the revisions we will make.

read point-by-point responses

  1. Referee: [Methods] Methods section (and abstract): The headline claims on RWI-driven vortex formation and strong suppression of planetesimal formation rest exclusively on the 2D vertically integrated equations; no 3D control runs or explicit justification is provided that vertical shear, buoyancy frequency, and dust sedimentation are adequately captured for linear growth rates and nonlinear vortex lifetime, which is load-bearing for the central claim.

    Authors: We acknowledge the limitation of using 2D vertically integrated simulations. This dimensionality was chosen to enable the high resolution and extended integration times required to follow vortex coalescence and multifluid dust evolution through the outburst and quiescent phases. Full 3D radiation-hydrodynamical runs with the same physics remain computationally prohibitive. We will revise the Methods section to include an explicit discussion of the 2D approximation, referencing prior work on the validity of vertically integrated models for RWI linear growth and nonlinear vortex evolution, while noting that vertical shear and buoyancy are expected to play a secondary role for the azimuthal dynamics studied here. We will also add a brief discussion of dust sedimentation effects. revision: partial

  2. Referee: [Results] Results (vortex diffusion and planetesimal suppression): The quantitative assertion that vortices 'strongly suppress' planetesimal formation via turbulent diffusion lacks reported convergence tests, resolution studies, or error analysis on the dust growth implementation, making the strength of the suppression difficult to evaluate independently.

    Authors: We agree that convergence and error analysis are needed to support the quantitative strength of the suppression claim. In the revised manuscript we will add a dedicated subsection presenting resolution studies at multiple grid sizes, together with an assessment of numerical convergence in the turbulent diffusion coefficient and its effect on the planetesimal formation threshold. revision: yes

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: results are direct outputs of described simulations

full rationale

The paper reports outcomes from high-resolution 2D vertically-integrated multifluid radiation-hydrodynamical simulations of disk outbursts. The central claims (RWI instability of the burst front, vortex coalescence, and suppression of planetesimal formation via turbulent diffusion) follow directly from the numerical evolution under the stated equations, opacity model, and initial conditions. No parameter fitting, self-definitional relations, or load-bearing self-citations are present that would make any result equivalent to its inputs by construction. The 2D setup is an explicit modeling choice whose limitations are external to circularity analysis.

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

Abstract-only review; no explicit free parameters, axioms, or invented entities are stated. Full text would be required to audit numerical choices such as opacity tables or dust growth prescriptions.

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Cite this review

Pith. "Pith review of Planet formation at the inner edge of the dead zone II. Outbursts, rings, vortices, and suppression of planetesimal formation." pith.science (2026). https://pith.science/paper/S7KJOZUO

@misc{pith2026260611344,
  author       = {Pith},
  title        = {Pith review of: Planet formation at the inner edge of the dead zone II. Outbursts, rings, vortices, and suppression of planetesimal formation},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/S7KJOZUO}},
  note         = {Machine review of arXiv:2606.11344}
}
read the original abstract

Accretion outbursts have been observed in a variety of young stellar objects, but models of their dynamical evolution have been largely limited to axisymmetric models due to their computational cost. We investigate the azimuthal stability of accretion outbursts and the formation of planetesimals during these events. We performed high-resolution 2D, vertically integrated multifluid radiation-hydrodynamical simulations of the inner 10 au of protoplanetary disks with a dynamically growing dust population, including radiation transport and a realistic dust opacity model. Accretion outbursts are highly unstable to the Rossby-wave instability, with the burst front quickly diffusing into a large number of small-scale vortices that coalesce over time into a single, compact vortex and inducing azimuthal asymmetries. Vortices act as a source of vigorous turbulent diffusion, strongly suppressing planetesimal formation. Our results suggest that azimuthal asymmetries associated with accretion outbursts should be both common and detrimental to planet formation. Nevertheless, planetesimal formation will resume post-burst, as the burst-induced vortices eventually decay and the disk returns to a quiescent state featuring a pressure bump at ~1 au.

Figures

Figures reproduced from arXiv: 2606.11344 by the authors.

Figure 1
Figure 1. Snapshot of our fiducial model (αDZ = 10−4 , vfrag = 1 m/s) at t = 20 yr, during the burst phase. Panels show the gas surface density Σg (a), temperature T (b), maximum grain size amax (c), and normalized vortensity ϖ/ϖ0 (d), with minima in the latter denoting the presence of vortices. The disk structure is highly nonaxisymmetric, with a dense crescent in Σg. theory, post-burst 20 50 100 200 500 1000 g [g/cm2 ] pre-… view at source ↗
Figure 2
Figure 2. Comparison between our fiducial model (orange lines) and an equivalent 1D model (blue, see paper I) at the end of the burst phase. The series of spikes in 1D gives way to smeared out radial profiles in the burst region in 2D. The analytical prediction for the shape of the post-burst region from paper I is shown with a thick gray line, and is in excellent agreement with the 2D model results. bump with a maximum at R … view at source ↗
Figure 4
Figure 4. Top: accretion rate M˙ acc onto the star as a function of time for our 2D models (solid lines) with αDZ = 10−4 (blue) and αDZ = 10−3 (orange), compared to their 1D counterparts (dashed lines). Both 1D and 2D models reach similar peak accretion rates, but 2D models exhibit a single accretion spike and a shorter burst duration. Bottom: the dust￾to-gas ratio of accreted material through the inner boundary, increasing d… view at source ↗
Figures from the paper (3 more)
Figure 6
Figure 6. Figure 6: Heatmaps of the perturbed vortensity in our high-resolution model over several snapshots, capturing the formation of vortices as the burst front reaches R ∼ 0.75 au (panels a–c) and their subsequent merging (d–j) until a single vortex has survived (panel k). Ellipses o…
Figure 7
Figure 7. Figure 7: Radius–time heatmaps of the azimuthally averaged turbulent viscosity α¯turb(R, t) for (top to bottom, left to right) our fiducial model with αDZ = 10−4 and vfrag = 1 m/s, a more diffusive model with αDZ = 10−3 , our high resolution model, and one with a higher fragment…
Figure 8
Figure 8. Figure 8: The maximum value of the azimuthally averaged Reynolds stress across the burst phase, as a tracer of the overall strength of vortex-driven turbulent stress. Dotted lines shows power-law fits to the data, with αvort ∝ R 0.55. The data is further smoothed with a rolling …

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Pith tools

Reviewed June 27, 2026 · model on record in the stance chip above.