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REVIEW 3 major objections 5 minor 73 references

Simulation of images of protoplanetary disks after collision with free-floating planets

T0 review · 3 major / 5 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read A 10-Jupiter-mass free-floating planet passing through a protoplanetary disk would leave a two-arm spiral if it moves with the disk's rotation and a one-arm spiral if it moves against it, along with a warped plane and a trailing gas…

desk verdict Clearly stated and potentially useful prediction (two vs one spiral arms for prograde vs retrograde flyby) but the grid is too coarse to support it; a convergence study is needed before trusting the arm-count claim. read the letter →

arxiv 2506.23795 v1 pith:JE2AT6OS submitted 2025-06-30 astro-ph.EP astro-ph.GAastro-ph.SR

Tatiana Demidova , Vitaliy Grigoryev This is my paper · ORCID
classification astro-ph.EPastro-ph.GAastro-ph.SR
keywords protoplanetarydisksfree-floatingplanetsplanet-diskinteractionnumericalsimulationspiralarmsradiativetransfersyntheticALMAobservationsparabolicflyby
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 argues that a close encounter between a ~10-Jupiter-mass free-floating planet and a protoplanetary disk would leave observable scars: spiral arms when the disk is viewed pole-on, a warped disk plane when viewed edge-on, and a gas tail following the planet. The authors simulate the gas-dynamic response of a 0.01-solar-mass disk to a planet on a parabolic orbit, then post-process the density fields with radiative transfer and an ALMA simulator to produce synthetic infrared and submillimeter images. They find that a prograde flyby (planet moving with the disk's rotation) produces two spiral arms, while a retrograde flyby produces one, with the difference tracing how the disk's rotation merges the two disturbances. The structures remain identifiable for roughly 500 years, which is short compared with disk lifetimes, but the scenario repeats if the planet is on a highly eccentric bound orbit that crosses the disk each periastron passage.

What carries the argument

The argument rests on a three-stage numerical pipeline. First, the PLUTO finite-volume code evolves the Euler equations with the star's potential plus a smoothed planetary potential (Klahr-Kley form) on a 144x60x144 spherical grid, with the planet on a fixed parabolic orbit—either prograde or retrograde relative to the disk's rotation. Second, RADMC-3D computes Monte Carlo radiative transfer through the resulting density field, assuming dust opacities for magnesium-iron silicates. Third, the CASA simulator turns the fluxes into synthetic ALMA images at 740 µm with realistic noise. The key physical mechanism is the gravitational wake: the planet raises two spiral humps at the two disk-plane crossings; the disk's rotation then determines whether the second hump survives as a separate arm (prograde) or merges into the first (retrograde). The diagnostic power comes from the one-arm/two-arm count, the warp asymmetry, and the trailing tail.

What would settle it

Target nearby young clusters with ALMA at 740 µm to search for disks with a single dominant spiral arm, an asymmetric warp, and a trailing gas tail. If surveys of several hundred disks in Taurus and Ophiuchus find no such morphology despite a substantial population of massive free-floating planets, the predicted ~500-year visibility window or the one-arm retrograde signature would be called into question.

Watch

Extended reading notes

Core claim

The central claim is that a 10-Jupiter-mass planet passing through a protoplanetary disk creates a specific, observationally identifiable morphology: two spiral density humps on the disk surface for a prograde encounter, one for a retrograde encounter, plus a warped disk plane and a trailing gas tail, all detectable in infrared (3 µm) and submillimeter (740 µm) images at distances of ~140 pc. The distinction between one and two arms arises because the planet intersects the disk plane twice; for retrograde motion the second hump merges with the first under the disk's rotation, whereas for prograde motion the two remain separate. Detectability requires a planet of at least 3 Jupiter masses and a fine-dust mass of roughly $10^{-4}$ solar masses; close flybys (pericenter ~5 AU) favor single-arm spirals, while more distant encounters (~20 AU) make double-arm spirals resolvable. The authors also show that the flyby does not change the disk's accretion rate onto the star.

Load-bearing premise

The planet is treated as a point mass on a fixed parabolic orbit, and the disk gas and the disk's self-gravity never push back on the planet, even though the disk's mass (0.01 solar masses) is about the same as the planet's (10 Jupiter masses).

Editorial extensions

If this is right

  • A pole-on image of a young disk with two bright spiral arms could be evidence of a recent prograde planetary flyby rather than an embedded planet or gravitational instability.
  • A single-arm spiral with a warped outer plane and a gas tail would point to a retrograde encounter, offering a way to infer the encounter geometry from a single snapshot.
  • The structures fade within ~500 years, so detections would imply either a very recent flyby or a planet on a highly eccentric bound orbit that re-intersects the disk every ~680 years, making repeated sightings possible.
  • ALMA Band 8 observations at ~140 pc can resolve the predicted spirals; single-arm spirals are best sought in close-flyby events, double-arm spirals in more distant passings.

Reading between the lines

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

  • If an eccentric bound planet re-encounters the disk every ~680 years, the one-arm and two-arm morphologies could appear repeatedly in the same object; a time series of images could then pin down the unseen planet's orbital period and pericenter.
  • The mass threshold of ~3 Jupiter masses implies that surveys for such scars should prioritize disks around stars in dense clusters, where massive free-floating planets are most common; a null detection in a large cluster sample would constrain the product of encounter rate and 500-year visibility time.
  • The computational domain truncates the gas tail, so its full length and detectability remain open; a follow-up simulation with a larger radial grid could test whether the tail is visible in CO or HI line emission, not just continuum.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 5 minor

Summary. The paper presents three-dimensional gas-dynamical simulations of a protoplanetary disk (0.01 M_sun) around a solar-mass star perturbed by a 10-Jupiter-mass free-floating planet on a parabolic orbit. Using the PLUTO code on a 144×60×144 spherical grid, the authors follow the disk response for about 500 years after the encounter, then post-process density distributions with RADMC-3D and the CASA simulator to produce synthetic infrared and submillimeter images. The central claim is that a prograde flyby produces two observable spiral arms in pole-on images, while a retrograde flyby produces a single arm, with additional signatures such as disk warping and a trailing gas tail. Variations in pericenter distance, inclination, argument of pericenter, and planet mass are explored, and the paper concludes that such structures are observable in nearby star-forming regions but persist for only ~500 years.

Significance. If correct, this work establishes a new, morphologically distinctive diagnostic for free-floating planet encounters with protoplanetary disks: the number and handedness of spiral arms would indicate the encounter geometry. The use of state-of-the-art radiative transfer and ALMA image synthesis makes the predictions falsifiable with current facilities. The paper also demonstrates that such structures persist only ~500 years, implying that frequent encounters (e.g., via highly eccentric bound planets) would be needed for detection. The strengths are the broad parameter scan, the use of publicly available validated codes (PLUTO, RADMC-3D, CASA), and the explicit synthetic observations. The main caveat is the absence of a resolution study and the simplified treatment of the planet's orbit and disk self-gravity, which bear directly on the headline result.

major comments (3)
  1. [Model and method / Results] The central one-arm versus two-arm discriminator is based on a single grid resolution of 144×60×144 cells over R∈[0.2,107.2] AU and θ∈[15°,165°]. In the region of interest (r≈5–20 AU), the vertical cell height is ~0.22–0.44 AU, while the disk pressure scale height H is ~0.34–0.8 AU; thus the disk thickness is resolved by only 1–2 cells. The Hill radius of a 10 M_Jup planet at 5 AU (~0.74 AU) is comparable to the radial cell width (~0.74 AU). The retrograde one-arm pattern is attributed to the second hump 'merging' with the first (Results, paragraph after Fig. 4), which could be a numerical diffusion artifact at this resolution. No convergence test or resolution study is presented. I request a resolution study, at least one higher-resolution run for the fiducial prograde and retrograde cases, to demonstrate that the arm count and merging behavior are converged.
  2. [Model and method] The planet is assumed to move on a fixed parabolic orbit, and disk self-gravity is neglected. The disk mass (0.01 M_sun) is ~10.5 M_Jup, almost identical to the planet mass (10 M_Jup). The gravitational back-reaction of the disk on the planet could decelerate or deflect the planet during its two disk-plane crossings, changing the epochs and locations of the hump excitation; self-gravity could also modify spiral wave propagation. Please provide an order-of-magnitude estimate of the dynamical friction or deflection timescale against the crossing time (~10^2 yr) to justify the fixed-orbit approximation, or quantify the effect on the predicted morphology.
  3. [Abstract / Results] The abstract claims that 'two spiral arms can be observed in case of the prograde fall, and one with retrograde case.' However, the Results state that 'In the inner part of the disk in both cases bright two-armed spirals are visible' (paragraph after Fig. 4). Thus the clean prograde/retrograde discriminator applies only to the outer part of the disk, or to the overall large-scale pattern, and not to the full pole-on image. Please reconcile the abstract with the detailed morphology and specify exactly which radial range or brightness level separates the two cases.
minor comments (5)
  1. [Table 1] Table 1 lists the unit of velocity as v0 = 4.74×10^5 cm s^-1 with the comment '2πL0/t0'; however, 2πL0/t0 = 2π × 1 AU / 1 year ≈ 2.98×10^6 cm s^-1, so the numerical value corresponds to L0/t0 without the factor 2π. Please correct the table or the value.
  2. [Initial and boundary conditions / Eq. (6)] The symbol ρ0 is used both as the normalization density (Table 1, 5.94×10^-7 g cm^-3) and as the midplane density scale in Eq. (6) and the subsequent text ('ρ0 = Σ0/√(2π) H0'). This double use is confusing; please rename one of them.
  3. [Image generation / Results (Fig. 8)] In the Image generation section, the total fine-dust mass is stated as ~2×10^-5 M_sun, but later the text says the structures can be observed 'if the mass of fine dust is at least 10^-4 M_sun'. Please clarify which dust mass was used for the images in Figs. 8 and 9 and reconcile the factor 5 difference.
  4. [Discussion / Conclusion] The tail of gas trailing the planet is claimed as a possible observable, but the authors note that 'due to the limited size of the computational domain, this tail is cut off'. As a result, the prediction for the tail's extent and brightness is incomplete; consider stating this caveat in the abstract or conclusions.
  5. [Results] The claim that the minimum planet mass for identifiable spirals is 3 M_Jup appears to be based on only two computed masses (1 and 10 M_Jup) plus possibly an intermediate run; please state the actual grid of masses used or rephrase as 'between 1 and 3 M_Jup' if no intermediate value was run.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: the predicted arm morphologies are emergent outputs of the PLUTO/RADMC-3D/CASA forward model, not encoded in any fitted input or self-citation.

full rationale

The paper's load-bearing claims (prograde flyby leaves a two-armed spiral, retrograde leaves one arm, warped disk plane, trailing gas tail, ~500 yr visibility, ALMA detectability) are all presented as results of a forward simulation chain: PLUTO gas dynamics, RADMC-3D radiative transfer, and CASA synthetic observations. The setup parameters (M* = 1 Msun, Md = 0.01 Msun, density profile from Nelson et al. 2013, inner temperature 1000 K, mp = 10 MJup, parabolic orbit with specified q, omega, and i) are literature-based or physically motivated; none encodes the arm count or morphology being predicted. No parameter is fitted to observational images or to the target structures. The one-arm/two-arm difference is described as an emergent outcome: 'in the case of a retrograde fall, the second hump merges with the first due to the rotation of the disk.' The self-citations (Grigoryev & Demidova 2024 for viscosity/thermal-conductivity coefficients, Demidova & Shevchenko 2015 for transient spirals in circumbinary disks, and Grigoryev & Demidova 2025 for UX Ori eclipses) are not used to import the central result or to forbid alternatives; they provide supporting method or context only. A reviewer concern that the 144x60x144 grid may under-resolve the disk scale height is a numerical convergence and robustness question, not circularity: even if the arm count were numerical, that would be an error, not a derivation that reduces to its own inputs by construction.

Assumptions & free parameters 8 free parameters · 6 assumptions · 0 invented entities

The central claim is an emergent numerical result, so the ledger contains no fitted parameters in the circularity sense, but it does enumerate the modeling choices (near-isothermal gas, prescribed planetary orbit, no self-gravity, no radiation feedback, and smoothing parameters) that the reader must accept to trust the predicted morphology. No new physical entities are introduced.

free parameters (8)
  • Planet mass mp = 10 MJup (also 1 MJup tested)
    Chosen as a representative massive free-floating planet; central detectability claim depends on it (minimum 3 MJup for observable spirals).
  • Pericenter distance q = 5 AU baseline; 10, 20 AU also run
    Controls how deep the planet penetrates and the brightness/lifetime of the arms; headline images use q = 5 AU.
  • Orbital inclination i = 10 deg baseline; 20 deg also run
    Affects time spent near the disk plane and arm brightness; headline images use i = 10 deg.
  • Argument of pericenter omega = 90 deg baseline; 0, 45, 135 deg also run
    Sets the radii of the two disk-plane crossings; affects which spiral branch is brighter.
  • Disk mass Md = 0.01 M_sun
    Chosen from Williams and Cieza (2011); sets density scale for image brightness and observability.
  • Adiabatic index gamma = 1.05
    Near-isothermal assumption; keeps temperature nearly constant and affects spiral wave propagation and shock structure.
  • Viscosity and thermal conductivity coefficients = not given; referenced to Grigoryev and Demidova (2024)
    Chosen to smooth the disk-corona transition and bow shocks; values not reproducible from this paper alone.
  • Smoothed potential radius Rsm = 0.03R
    Softening length for the planet's gravity; affects the gravitational torque near the planet and depends on radius.
assumptions (6)
  • domain assumption The ideal-gas hydrodynamics with gamma = 1.05 and a maintained temperature profile capture the disk response to the planet.
    Used in Eqs. (1)-(5); radiation transfer, dust-gas interaction, and self-gravity are explicitly ignored, so the gas response is approximate.
  • domain assumption The planet travels on a fixed parabolic orbit, unaffected by gas drag or disk gravity.
    The potential (3) includes only the planet's gravity on the gas; no equation of motion for the planet is solved, even though the disk mass is comparable to the planet mass.
  • domain assumption Disk self-gravity is negligible.
    Stated in the Model section. With Md = 0.01 M_sun, self-gravity may not be negligible at large radii.
  • domain assumption The smoothed planet potential (3) with Rsm = 0.03R represents a 10 MJup planet at the chosen resolution.
    The softening length is a significant fraction of the Hill sphere at small radii and weakens the planet's gravitational interaction.
  • domain assumption Initial density (6), sound speed (7), and angular velocity (9) describe a realistic disk.
    Set by p = -2.25, q = -0.5, H0 and T0 = 1000 K at rin = 0.2 AU, following Nelson et al. (2013).
  • domain assumption Mie-theory dust opacities with sub-Rayleigh grains and fixed dust mass yield representative images.
    Used in RADMC-3D and CASA; assumes no dust growth or settling during the 500-year simulation.

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Cite this review

Pith. "Pith review of Simulation of images of protoplanetary disks after collision with free-floating planets." pith.science (2026). https://pith.science/paper/JE2AT6OS

@misc{pith2026250623795,
  author       = {Pith},
  title        = {Pith review of: Simulation of images of protoplanetary disks after collision with free-floating planets},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/JE2AT6OS}},
  note         = {Machine review of arXiv:2506.23795}
}
read the original abstract

Observational manifestations of disturbances in a protoplanetary disk caused by a collision with a massive planet are studied. It is assumed that the planet moves along a parabolic trajectory that intersects the disk plane near the star. Gas-dynamic simulation is performed using the finite volume method on a long time scale. On its basis, images of the disk observed from the pole and edge-on are constructed in the infrared and submillimeter ranges. A wide range of planet orbit parameters is considered. The approach of the planet was considered both prograde and retrograde with the respect to the disk rotation. Calculations have shown that in the images of the disk seen pole-on, two spiral arms can be observed in case of the prograde fall, and one with retrograde case. In the case of observations of a disk whose plane is inclined at a small angle to the line of sight, distortions of the disk plane can be noticeable. In addition, a gas tail is extended from the disk in the direction of the planet's motion, which can also be identified in observations.

Figures

Figures reproduced from arXiv: 2506.23795 by the authors.

Figure 1
Figure 1. Surface of maximum density at the time 290 years relative to the start of calculations in the model q = 5 AU, ω = 90◦ , i = 10◦ . The case of a prograde flyby is shown at the top, and a retrograde one at the bottom. The color shows the density in units of ρ0 = 6 × 10−7 g cm−3 . The coordinate parallelepiped is shown for scale. flybys of the planet. The decrease in the visible size of the disk at the moment of 290 ye… view at source ↗
Figure 2
Figure 2. The color shows the product of the radiation flux at a wavelength of 3 µm and the square of the distance for the case of a prograde fall of the planet onto the disk. Model parameters: q = 5 AU, ω = 90◦ , i = 10◦ . The time moment t = 200 years from the beginning of the calculations is shown on the left, t = 290 years is shown in the center, and t = 500 years is shown on the right. The upper graphs correspond to the … view at source ↗
Figure 3
Figure 3. The same as in [PITH_FULL_IMAGE:figures/full_fig_p011_3.png] view at source ↗
Figures from the paper (6 more)
Figure 4
Figure 4. Figure 4: The same as in [PITH_FULL_IMAGE:figures/full_fig_p012_4.png]
Figure 5
Figure 5. Figure 5: Same as in [PITH_FULL_IMAGE:figures/full_fig_p012_5.png]
Figure 6
Figure 6. Figure 6: Same as in [PITH_FULL_IMAGE:figures/full_fig_p013_6.png]
Figure 7
Figure 7. Figure 7: The same as in [PITH_FULL_IMAGE:figures/full_fig_p013_7.png]
Figure 8
Figure 8. Figure 8: The color shows the radiation flux at a wavelength of 740 µm in a logarithmic scale at time t = 290 years. On the left is a prograde flyby for the model with parameters: q = 20 AU, i = 10◦ , ω = 90◦ , and on the right is a retrograde one for the model: q = 5 AU, i = 10…
Figure 9
Figure 9. Figure 9: The synthesized images that could potentially be obtained with the ALMA radio interfer￾ometer at a wavelength of 740 µm correspond to the models presented in [PITH_FULL_IMAGE:figures/full_fig_p015_9.png]

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Reviewed August 6, 2026 · model on record in the stance chip above.