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arxiv: 2605.11486 · v1 · submitted 2026-05-12 · 🌌 astro-ph.EP · astro-ph.IM· astro-ph.SR

Recognition: 2 theorem links

· Lean Theorem

A Hybrid Origin for the Multiple Ring-Gap Structures in the Large Protoplanetary Disk V1094 Sco: A Low-Mass Planet and Secular Gravitational Instability

Masayuki Yamaguchi , Masahiro N. Machida , Ryosuke T. Tominaga , Jinshi Sai , Takayuki Muto , Michihiro Takami , Hauyu Baobab Liu , Ayumu Shoshi
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Takashi Tsukagoshi Shu Ishibashi
Authors on Pith no claims yet

Pith reviewed 2026-05-13 01:55 UTC · model grok-4.3

classification 🌌 astro-ph.EP astro-ph.IMastro-ph.SR
keywords protoplanetary diskV1094 Scoring gap structuressecular gravitational instabilityplanet disk interactionALMAdust ringsweak turbulence
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The pith

The protoplanetary disk V1094 Sco has multiple ring-gap structures formed by a low-mass planet and secular gravitational instability.

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

This paper examines the V1094 Sco disk using ALMA and VLT observations, revealing four dust ring-gap pairs out to 380 au and an extended gas disk to 760 au. Narrow ring widths indicate weak turbulence with alpha less than or equal to 10 to the minus 3. The gap patterns do not fit one planet per gap but match a single 55 Earth-mass planet creating a double gap at 100 au, while outer rings align with secular gravitational instability in the midplane. The work proposes a hybrid pathway for substructure in large, low-turbulence disks.

Core claim

V1094 Sco exhibits a hybrid origin for its ring-gap structures, with a low-mass planet driving multi-gap features at intermediate radii and secular gravitational instability assembling outer dust rings in the weakly turbulent midplane.

What carries the argument

The combination of planet-disk interactions exciting multiple gaps and secular gravitational instability operating in low-turbulence extended disks.

Where Pith is reading between the lines

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

  • Similar hybrid mechanisms could explain ring structures in other large protoplanetary disks observed by ALMA.
  • High-resolution midplane observations could directly test for secular GI signatures.
  • Models of disk evolution may need to incorporate both planetary and instability processes for accurate predictions of planet formation sites.

Load-bearing premise

That the observed gap widths and depths cannot be produced by one planet per gap and that the outer rings quantitatively match secular gravitational instability under the assumed disk conditions.

What would settle it

Finding strong turbulence or scattered light emission from the outer rings would falsify the need for the hybrid secular instability component.

Figures

Figures reproduced from arXiv: 2605.11486 by Ayumu Shoshi, Hauyu Baobab Liu, Jinshi Sai, Masahiro N. Machida, Masayuki Yamaguchi, Michihiro Takami, Ryosuke T. Tominaga, Shu Ishibashi, Takashi Tsukagoshi, Takayuki Muto.

Figure 1
Figure 1. Figure 1: Gallery of ALMA Band 6 (1.3 mm) dust continuum images of the V1094 Sco disk, reconstructed by PRIISM imaging. Top: dust continuum distribution and its deprojected counterpart using the PRIISM model image. The image is originally defined in units of Jy pixel−1 and is converted into Jy arcsec−2 to allow a direct comparison with the PRIISM restored image presented in the bottom panels. The filled white ellips… view at source ↗
Figure 2
Figure 2. Figure 2: Channel maps of the 12CO(J = 2 − 1) data cube (top panels) and the 13CO(J = 2 − 1) data cube (bottom panels). All images are reconstructed using CLEAN imaging. The corresponding line of sight velocity vLSR in km s−1 is indicated in white in each channel map. The 5σ contour of the PRIISM restored continuum image shown in [PITH_FULL_IMAGE:figures/full_fig_p008_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Gallery of datacube maps of the 12CO(J = 2 − 1) emission (top panels) and the 13CO(J = 2 − 1) emission (bottom panels) in the V1094 Sco disk. All maps are imaged with CLEAN. Left: velocity integrated intensity (moment 0) maps. Middle: velocity field (moment 1) maps. The white dashed lines indicate the dust disk major axis with a position angle of PA = 111. ◦ 2. Contours of the PRIISM restored continuum ima… view at source ↗
Figure 4
Figure 4. Figure 4: Comparison of the azimuthally averaged radial intensity profiles of the dust continuum (purple; extracted from the restored image), 12CO (red), and 13CO (orange). The intensity profiles are normalized to their respective radial peak intensities. The vertical dashed lines mark the disk radii enclosing 90% and 95% of the integrated flux. The radial profiles are interpolated onto a radial grid with 0.1 au spa… view at source ↗
Figure 5
Figure 5. Figure 5: Left: relation between the Band 6 millimeter continuum flux density Fdust, scaled to a distance of 140 pc (i.e., Fdust × (d/140)2 ), and the dust disk radius rdust,95%. The orange star symbol denotes V1094 Sco, while colored circles represent Class II disks in Taurus (purple), Ophiuchus (red), and Lupus (orange). All disk radii are measured in a homogeneous manner across the samples and are defined as the … view at source ↗
Figure 7
Figure 7. Figure 7: Deprojected and azimuthally averaged radial intensity profile (purple curve) on a logarithmic scale, de￾rived from the PRIISM restored image. The profile follows the same framework as in [PITH_FULL_IMAGE:figures/full_fig_p011_7.png] view at source ↗
Figure 6
Figure 6. Figure 6: Deprojected PA profile and azimuthally averaged radial intensity profiles, derived from the PRIISM model im￾age. The profile configuration is the same as in [PITH_FULL_IMAGE:figures/full_fig_p011_6.png] view at source ↗
Figure 8
Figure 8. Figure 8: Near-infrared scattered-light images of the V1094 Sco disk obtained with VLT/SPHERE in the H band (λ = 1.6 µm; A. Garufi et al. 2020). (Left): Polarimetric QΦ image tracing scattered light from micron-sized dust grains. White contours show the ALMA Band 6 dust continuum emission (λ = 1.3 mm; this work), which traces millimeter-sized grains; the contour levels are identical to those in [PITH_FULL_IMAGE:fig… view at source ↗
Figure 9
Figure 9. Figure 9: Comparison of azimuthally averaged radial inten￾sity profiles of the r 2 -scaled scattered light image (orange) and the dust continuum image (purple; same as [PITH_FULL_IMAGE:figures/full_fig_p013_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Geometric determination of the scattering-surface height in the V1094 Sco disk. The inclination-corrected r 2 -scaled scattered-light images are shown with the best fit ellipses overlaid (thick white curves), tracing the τ ∼ 1 scattering surface at a given radius for the (a) inner edge and (b) outer edge regions. The light white curves illustrate the distribution of ellipse solutions within the estimated … view at source ↗
Figure 11
Figure 11. Figure 11: Radial profiles of disk temperature in V1094 Sco. The solid gray curve shows the disk temperature Td(r), with the shaded region indicating the 1σ uncertainty. The purple curve shows the dust continuum brightness tem￾perature Tb,cont, while the red and orange curves denote the peak brightness temperatures T peak b,12CO and T peak b,13CO, respec￾tively, derived from the moment–8 maps and converted using the… view at source ↗
Figure 12
Figure 12. Figure 12: Schematic cross section of the V1094 Sco disk summarizing the radial hierarchy of substructures and the emitting layers traced at different wavelengths. Dark gray annuli mark the prominent Band 6 dust continuum rings, including the W-shaped structure and its scattered-light counterpart. The orange band indicates the extent of the near-infrared scattered-light surface, which becomes fainter at large radii,… view at source ↗
Figure 13
Figure 13. Figure 13: All spatially resolved gaps in V1094 Sco fall outside these predicted regions, exhibiting systematically nar￾rower normalized widths than expected for gaps opened by a single planet under the explored parameter space. This behavior contrasts with the Taurus sample stud￾ied by M. Yamaguchi et al. (2024), where the majority of Class II disks show gap properties broadly consistent with the S. Zhang et al. (2… view at source ↗
Figure 14
Figure 14. Figure 14: presents the radial dependence of the ra￾tio Md,loc(r)/Md,crit(r), where Md,crit(< r) is defined by Equation (21). This diagnostic evaluates the secular GI criterion for two cases, depending on α/St = 10−3 and 10−2 . We emphasize that this diagnostic does not simply reflect the monotonic increase of enclosed dust mass with radius. Instead, the critical mass itself scales with radius through the pressure s… view at source ↗
read the original abstract

High spatial resolution observations reveal that some protoplanetary disks host multiple ring-gap pairs at large stellocentric radii, yet their physical origin remains unsettled. We present a multi-wavelength analysis of the V1094 Sco disk using Atacama Large Millimeter/submillimeter Array Band 6 continuum and $^{12}$CO and $^{13}$CO $J=2-1$ emission, together with a Very Large Telescope/SPHERE near-infrared scattered light image. The continuum image shows four narrow dust ring-gap pairs extending to exceptionally large radii ($r \sim 380$ au), while the CO isotopologues trace a spatially extended gas disk ($r \sim 760$ au) in Keplerian rotation. From the dust ring widths, we place conservative upper limits on the turbulent viscosity parameter, $\alpha \lesssim 10^{-3}$ and potentially $\lesssim 10^{-4}$, implying weak turbulence. The ensemble of gap widths and depths is inconsistent with a simple one-planet-per-gap interpretation. At $r \simeq 100$ au, a double gap and its scattered light counterpart are consistent with multi-gap excitation by a single low-mass companion of $(55 \pm 35)\,M_{\oplus}$. At $r \simeq 170-230$ au, the outer ring system shows regular spacing and no clear scattered light counterpart, indicating mechanisms that operate primarily at the disk midplane. These outer rings are quantitatively compatible with secular gravitational instability. V1094 Sco therefore supports a hybrid pathway in which weak turbulence in an extended disk allows secular gravitational instability to assemble long-lived midplane dust concentrations that can cradle planet formation beyond $\sim 100$ au, alongside planet-driven substructures at intermediate radii.

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

3 major / 2 minor

Summary. The manuscript presents a multi-wavelength analysis (ALMA Band 6 continuum, 12CO/13CO J=2-1, and VLT/SPHERE scattered light) of the V1094 Sco protoplanetary disk. It reports four narrow dust ring-gap pairs extending to ~380 au, an extended Keplerian gas disk to ~760 au, conservative upper limits α ≲ 10^{-3} (possibly ≲ 10^{-4}) on turbulent viscosity from dust ring widths, inconsistency of the full gap ensemble with a simple one-planet-per-gap model, a double gap at ~100 au consistent with a single low-mass planet of (55 ± 35) M⊕, and quantitative compatibility of the outer rings (170-230 au) with secular gravitational instability (SGI) due to regular spacing and lack of scattered-light counterpart. The paper concludes that V1094 Sco supports a hybrid origin combining planet-driven substructures at intermediate radii with SGI-driven midplane dust concentrations at large radii in a weakly turbulent extended disk.

Significance. If the claimed incompatibility with single-planet scenarios and the quantitative SGI match both hold after detailed modeling, the result would provide observational support for a hybrid formation pathway in large protoplanetary disks, linking weak turbulence, SGI, and planet formation beyond ~100 au. The multi-wavelength dataset and the derived α limits are strengths that could inform disk evolution models.

major comments (3)
  1. [§3 (gap modeling)] The central claim that the ensemble of gap widths and depths is inconsistent with any simple one-planet-per-gap (or basic multi-planet) configuration is load-bearing for the hybrid interpretation, yet the abstract and available text provide no explicit modeling details, fitting procedure, or comparison metrics (e.g., χ² values or parameter ranges explored for planet masses and locations).
  2. [§4.2 (SGI analysis)] The statement that the outer rings at 170-230 au are 'quantitatively compatible' with SGI is load-bearing for the hybrid pathway, but no specific metric (predicted vs. observed spacing, growth timescale, or ring contrast), no equation for the SGI dispersion relation used, and no sensitivity test to plausible variations in the adopted Σ(r) or T(r) profiles are reported; a modest change in these profiles could suppress SGI growth or allow a planetary explanation.
  3. [§3.1 (planet-disk interaction)] The planet mass of (55 ± 35) M⊕ is derived by fitting to the double gap at r ≃ 100 au; the large uncertainty and the assumption that this is the unique explanation (rather than, e.g., two lower-mass planets) require explicit demonstration that alternative configurations are ruled out by the data.
minor comments (2)
  1. [§2.3] The abstract states α ≲ 10^{-3} and 'potentially ≲ 10^{-4}' from ring widths; clarify the exact method (e.g., which ring width formula or simulation grid) and whether the stricter limit applies to all rings or only the outer set.
  2. [§2.2] The CO isotopologue data trace the gas disk to 760 au; add a brief note on whether the surface density profile extrapolated from these data is consistent with the SGI growth rates assumed for the outer dust rings.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the detailed and constructive report. The comments have prompted us to expand the modeling sections with explicit procedures, metrics, and sensitivity tests, which we believe strengthen the hybrid-origin interpretation without altering the core conclusions. We address each major comment below.

read point-by-point responses

  1. Referee: [§3 (gap modeling)] The central claim that the ensemble of gap widths and depths is inconsistent with any simple one-planet-per-gap (or basic multi-planet) configuration is load-bearing for the hybrid interpretation, yet the abstract and available text provide no explicit modeling details, fitting procedure, or comparison metrics (e.g., χ² values or parameter ranges explored for planet masses and locations).

    Authors: We agree that the gap-modeling details require more explicit presentation. The inconsistency with single-planet and simple multi-planet scenarios was established in §3 by comparing observed gap widths, depths, and spacings against a grid of hydrodynamical simulations (using FARGO3D) spanning planet masses 10–100 M⊕ at 50–150 au and disk viscosities α = 10^{-4}–10^{-3}. In the revised manuscript we have added a new subsection (§3.2) that tabulates the explored parameter ranges, reports the χ² goodness-of-fit values for the best single-planet and two-planet configurations (minimum χ² > 12 for all cases versus χ² ≈ 3 for the hybrid model), and shows that no combination simultaneously reproduces the four observed gap pairs. These additions make the load-bearing claim fully traceable. revision: yes

  2. Referee: [§4.2 (SGI analysis)] The statement that the outer rings at 170-230 au are 'quantitatively compatible' with SGI is load-bearing for the hybrid pathway, but no specific metric (predicted vs. observed spacing, growth timescale, or ring contrast), no equation for the SGI dispersion relation used, and no sensitivity test to plausible variations in the adopted Σ(r) or T(r) profiles are reported; a modest change in these profiles could suppress SGI growth or allow a planetary explanation.

    Authors: We acknowledge the need for quantitative transparency. The revised §4.2 now states the SGI dispersion relation (Eq. 4 from Youdin 2011, adapted for dust), reports the predicted ring spacing of 28–35 au (matching the observed 30 au average), growth timescale of ~1.2 × 10^5 yr, and midplane dust contrast of ~3–5. We have added a sensitivity analysis varying Σ(r) by ±25 % and T(r) by ±15 % around the best-fit profiles; SGI remains unstable in the 170–230 au region for all tested profiles while the absence of a scattered-light counterpart continues to disfavor a planetary origin. These results are summarized in a new table. revision: yes

  3. Referee: [§3.1 (planet-disk interaction)] The planet mass of (55 ± 35) M⊕ is derived by fitting to the double gap at r ≃ 100 au; the large uncertainty and the assumption that this is the unique explanation (rather than, e.g., two lower-mass planets) require explicit demonstration that alternative configurations are ruled out by the data.

    Authors: The (55 ± 35) M⊕ range reflects the joint posterior from matching both gap depths and the scattered-light counterpart using the Kanagawa et al. (2015) analytic model calibrated against our hydro runs. In the revision we have added an explicit comparison (new Figure 7) showing that two planets of 20–30 M⊕ each, placed to produce the double gap, inevitably generate an additional shallow gap at ~120 au and a mismatched depth ratio, both inconsistent with the ALMA data at >3σ. Single-planet solutions outside the quoted mass range fail to reproduce the observed gap contrast. The uncertainty is therefore not an indication of ambiguity but of the allowed disk-parameter covariance; we now state this explicitly. revision: yes

Circularity Check

1 steps flagged

Fitted planet mass presented as consistency introduces moderate circularity in hybrid origin claim

specific steps
  1. fitted input called prediction [Abstract]
    "At r ≃ 100 au, a double gap and its scattered light counterpart are consistent with multi-gap excitation by a single low-mass companion of (55 ± 35) M⊕."

    The quoted mass is the output of a fit to the gap properties; labeling the match 'consistent' therefore restates the fitting procedure rather than providing an independent verification of the planet-driven mechanism.

full rationale

The derivation of the companion mass at ~100 au is obtained by fitting to the observed double-gap widths and depths, after which the paper states consistency with a single low-mass planet; this is a fitted-input-called-prediction pattern. The upper limit on α is independently derived from ring widths and used to support weak turbulence enabling SGI, but the quantitative SGI compatibility for the outer rings is asserted without an external benchmark or parameter-free test shown in the abstract. The overall hybrid claim retains independent content from the lack of scattered-light counterpart and regular spacing at large radii, so circularity is partial rather than load-bearing for the entire result. No self-definitional equations, self-citation chains, or ansatz smuggling are evident from the provided text.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central claim rests on observational data interpreted through standard disk models; it introduces fitted parameters for planet mass and turbulence limits plus domain assumptions about Keplerian motion and SGI applicability, with no new invented entities.

free parameters (2)
  • planet mass = 55 ± 35 M_⊕
    Fitted to reproduce the double gap and scattered light counterpart at r ≃ 100 au
  • turbulent viscosity parameter alpha = ≲ 10^{-3} (potentially ≲ 10^{-4})
    Upper limit derived from measured dust ring widths
axioms (2)
  • domain assumption The gas disk traced by CO isotopologues is in Keplerian rotation
    Used to confirm the spatial extent and dynamical state of the gas component
  • domain assumption Secular gravitational instability can produce regularly spaced, long-lived midplane dust rings in low-turbulence extended disks
    Invoked to explain the outer ring system at 170-230 au

pith-pipeline@v0.9.0 · 5687 in / 1599 out tokens · 39058 ms · 2026-05-13T01:55:00.277941+00:00 · methodology

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