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arxiv: 2605.11486 · v2 · pith:SYHAQTOZnew · submitted 2026-05-12 · 🌌 astro-ph.EP · astro-ph.IM· astro-ph.SR

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
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Pith reviewed 2026-06-30 22:43 UTC · model grok-4.3

classification 🌌 astro-ph.EP astro-ph.IMastro-ph.SR
keywords protoplanetary disksring-gap structuressecular gravitational instabilityplanet formationV1094 ScoALMA observationsdisk substructuresweak turbulence
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The pith

The ring-gap structures in the V1094 Sco disk arise from a low-mass planet creating gaps near 100 au together with secular gravitational instability forming the outer rings at 170-230 au.

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

The paper examines multi-wavelength data on the unusually large V1094 Sco protoplanetary disk to determine why it shows four narrow dust ring-gap pairs out to 380 au. Analysis of gap widths and depths rules out a single planet explaining every feature, while the inner double gap matches excitation by one companion of roughly 55 Earth masses and the outer rings show regular spacing with no scattered-light signal. Weak turbulence throughout the disk, with viscosity parameter alpha at most 10 to the minus 3, allows secular gravitational instability to concentrate dust at the midplane for the outer rings. A reader would care because the result points to distinct formation routes operating at different distances in the same disk, including a path for dust concentrations to form far from the star.

Core claim

The authors conclude that V1094 Sco supports a hybrid origin in which a low-mass planet of 55 plus or minus 35 Earth masses produces the double gap near 100 au while secular gravitational instability assembles the outer ring system between 170 and 230 au. The gas disk extends to 760 au in Keplerian rotation, but the dust rings reach only 380 au, with upper limits on turbulent viscosity of alpha less than or equal to 10 to the minus 3 and possibly 10 to the minus 4. The outer rings lack a scattered-light counterpart and exhibit spacing incompatible with planet gaps alone, while the full set of gap properties is inconsistent with one planet per gap across the disk.

What carries the argument

Secular gravitational instability, which concentrates dust into long-lived midplane rings in weakly turbulent gas disks.

If this is right

  • A single low-mass planet can produce multiple gaps at intermediate radii while secular gravitational instability operates separately at larger radii.
  • Weak turbulence with alpha less than or equal to 10 to the minus 3 permits secular gravitational instability to create stable dust concentrations beyond 100 au.
  • The modeling of gap widths and depths across the disk rules out any simple one-planet-per-gap scenario for the full structure.
  • Long-lived midplane dust concentrations assembled by secular gravitational instability can serve as sites for planet formation at large stellocentric distances.

Where Pith is reading between the lines

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

  • Other extended disks with low turbulence may exhibit similar outer rings if observed at comparable resolution, suggesting the hybrid pattern is not unique to V1094 Sco.
  • Direct measurements of midplane dust concentrations in additional large disks could test whether secular gravitational instability commonly operates beyond the reach of planet-driven gaps.
  • The coexistence of the two mechanisms implies that planet formation models must incorporate both dynamical excitation by companions and instability-driven dust trapping at different radii.

Load-bearing premise

The outer rings at 170-230 au form via secular gravitational instability rather than planets, based on their regular spacing and absence of a scattered-light counterpart.

What would settle it

Detection of scattered light from the outer rings or a turbulence measurement showing alpha greater than 10 to the minus 3 across the outer disk would falsify the secular gravitational instability interpretation.

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 $\sim100$~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

1 major / 3 minor

Summary. The manuscript presents a multi-wavelength analysis (ALMA Band 6 continuum and CO isotopologues plus VLT/SPHERE NIR scattered light) of the V1094 Sco protoplanetary disk. It identifies four narrow dust ring-gap pairs extending to ~380 au within a gas disk reaching ~760 au, derives conservative upper limits α ≲ 10^{-3} (potentially ≲ 10^{-4}) on turbulent viscosity from ring widths, shows that the full set of gap widths and depths is inconsistent with a simple one-planet-per-gap model, attributes the double gap near 100 au to multi-gap excitation by a single 55 ± 35 M_⊕ companion, and finds the outer rings (170–230 au) quantitatively compatible with secular gravitational instability on the basis of regular spacing, absence of a scattered-light counterpart, and the low-α environment. The central claim is a hybrid origin combining planet-driven substructures at intermediate radii with SGI-driven midplane dust concentrations at large radii.

Significance. If the hybrid interpretation is upheld, the result supplies direct observational support for secular gravitational instability operating in extended, low-turbulence disks beyond ~100 au, thereby broadening the set of viable pathways for dust concentration and planet formation at large stellocentric distances. The multi-wavelength separation of midplane versus surface processes and the quantitative exclusion of a single-mechanism explanation constitute concrete advances that can be tested against future higher-resolution data or numerical simulations of SGI growth rates.

major comments (1)
  1. [Gap modeling and planet-mass section] Gap-width and depth modeling (the section deriving the 55 ± 35 M_⊕ planet mass and ruling out one-planet-per-gap across the full radial range): the large uncertainty interval on planet mass must be propagated through the multi-gap excitation calculation to demonstrate that a single companion remains viable over the full 20–90 M_⊕ range; otherwise the inconsistency claim for the outer gaps rests on a point estimate.
minor comments (3)
  1. [Turbulence limits paragraph] The abstract states α ≲ 10^{-3} and 'potentially ≲ 10^{-4}'; the main text should explicitly map which individual ring widths produce the tighter bound and whether the same α applies to the outer SGI region.
  2. [Outer rings figure] Figure showing the outer ring system (170–230 au): the radial spacing measurement and the quantitative SGI wavelength comparison should be presented in a dedicated panel or table with the adopted surface-density and temperature profiles.
  3. [Discussion of outer rings] The SGI compatibility statement would benefit from a short sensitivity test (varying α within the derived upper limit) to show that the growth-rate match is not confined to a single parameter choice.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for the detailed and constructive report. The single major comment concerns propagation of the planet-mass uncertainty through the multi-gap modeling; we address it directly below and will incorporate the requested analysis in the revised manuscript.

read point-by-point responses

  1. Referee: [Gap modeling and planet-mass section] Gap-width and depth modeling (the section deriving the 55 ± 35 M_⊕ planet mass and ruling out one-planet-per-gap across the full radial range): the large uncertainty interval on planet mass must be propagated through the multi-gap excitation calculation to demonstrate that a single companion remains viable over the full 20–90 M_⊕ range; otherwise the inconsistency claim for the outer gaps rests on a point estimate.

    Authors: We agree that the full 20–90 M_⊕ range must be shown explicitly rather than relying on the central value. In the revised manuscript we will recompute the multi-gap excitation models at the lower (20 M_⊕) and upper (90 M_⊕) bounds, confirming that a single companion can still account for the double gap near 100 au across the entire interval while the outer gaps at 170–230 au remain inconsistent with the same mechanism. This additional calculation will be presented in an expanded figure and accompanying text. revision: yes

Circularity Check

0 steps flagged

No significant circularity; derivation relies on independent morphological and multi-wavelength constraints

full rationale

The paper's central claims rest on direct comparison of observed gap widths/depths and ring spacing against standard planet-disk interaction models and SGI wavelength predictions, using ALMA and SPHERE data as inputs. No equations reduce a claimed prediction to a fitted parameter by construction, no self-citation chain supplies a uniqueness theorem, and no ansatz is smuggled via prior work. The hybrid pathway conclusion follows from the radial separation of features (planet-like at ~100 au vs. midplane-only at 170-230 au) without self-referential redefinition of observables.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

The central claim rests on standard disk modeling assumptions and one fitted parameter for planet mass; no new entities are introduced.

free parameters (1)
  • planet mass = 55 ± 35 M_⊕
    Derived from matching the double gap at r ≃ 100 au to multi-gap excitation by a single companion
axioms (2)
  • domain assumption The gas disk is in Keplerian rotation as traced by CO isotopologues
    Used to establish the spatial extent and dynamical state of the disk
  • domain assumption Dust ring widths imply turbulent viscosity parameter α ≲ 10^{-3}
    Conservative upper limits placed from observed ring widths to support weak turbulence

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