Circumstellar and circumbinary discs in multiple stellar systems

Antoine Alaguero; Nicol\'as Cuello; Pedro P. Poblete

Circumstellar and circumbinary discs in multiple stellar systems

T0 review · 0 major / 6 minor · reviewed 2026-08-09 · deepseek-v4-flash

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Pith's one-line read Stellar companions systematically reshape the protoplanetary discs in which planets form.

desk verdict Competent, well-referenced review of discs in multiple-star systems; the genuinely new material is the compiled catalogue and uniform image gallery, but the synthesis leans on the standard binary-torque cavity scaling without quantifying how often it actually holds. read the letter →

arxiv 2501.19249 v1 pith:GHOEEZ5A submitted 2025-01-31 astro-ph.EP astro-ph.SR

Nicolás Cuello , Antoine Alaguero , Pedro P. Poblete This is my paper · ORCID

classification astro-ph.EPastro-ph.SR

keywords protoplanetarydiscsstellarmultiplicitycircumbinarycircumstellartidaltruncationdiscmisalignmentdusttrapsplanetformation

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 review argues that most stars are born with companions, and those companions are not a side note for planet formation: they decisively reshape the discs out of which planets grow. Across circumstellar discs, a nearby star truncates the outer disc, steepens its density profile, and accelerates the inward drift of dust; around binaries, the central stars empty a large cavity and concentrate solids at its edge. The paper brings together imaging of systems such as HT Lup, HD 100453, GG Tau, GW Ori, HD 142527, and HD 98800 with hydrodynamic simulations to make the case that truncation, spirals, and misalignment are the rule rather than the exception. If the synthesis is right, planet formation in multiple stellar systems is systematically different: smaller discs, shorter lifetimes, and planetary systems with inclined or polar orbits. The review's own contribution is the synthesis and the comparison gallery of ALMA and SPHERE images, not new measurements.

What carries the argument

The load-bearing mechanism is the gravitational torque between stars and disc, applied at Lindblad resonances. For circumstellar discs, the companion's torque truncates the disc at a radius set by the binary separation and mass ratio; for circumbinary discs, the resonant torques of the inner binary open a central cavity, typically two to three times the binary separation for circular orbits and larger for eccentric binaries, and launch spiral density waves. The companion's eccentricity and inclination determine whether the disc precesses, breaks, or settles into a polar configuration. A second mechanism is aerodynamic dust drift: a steeper pressure gradient in truncated discs speeds radial drift, while pressure bumps at cavity edges and spiral arms act as dust traps where solids can concentrate and grow.

What would settle it

A statistically complete ALMA survey of a young star-forming region that found circumstellar disc sizes uncorrelated with companion separation, or circumbinary discs whose cavities show no edge dust concentration, would break the claim that multiplicity systematically truncates discs and traps solids. Concretely, if discs in binaries with measured orbits were routinely larger than the predicted truncation radius, the standard torque theory would need revision.

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Extended reading notes

Core claim

The central claim is that stellar multiplicity alters the dynamics and morphology of protoplanetary discs in three linked ways: tidal truncation, misalignment, and dust trapping. Circumstellar discs around individual stars in a binary are cut back by the companion's torque, so they are smaller, steeper, and shorter-lived than discs around single stars. Circumbinary discs are carved from the inside by the binary, whose resonant torques open a cavity a few times the binary separation and, for eccentric binaries, make the cavity eccentric and lopsided; the cavity edge is a pressure maximum that traps dust and can seed planetesimals. Misaligned configurations produce warps, disc tearing, and, around eccentric binaries, polar discs orthogonal to the binary plane. The paper argues these are not exotic outcomes but generic consequences of the fact that roughly 65 percent of stars form in multiple systems.

Load-bearing premise

The synthesis assumes the cited observations and simulations are accurate and representative, and that standard resonant-truncation theory, developed from idealized binary-disc simulations, transfers to real discs with realistic thermodynamics, viscosity, and dust content.

Editorial extensions

If this is right

Disc sizes and lifetimes are systematically reduced in binary systems, shrinking the available mass budget for gas-giant formation.
Solids collect at the edges of circumbinary cavities, so planetesimal formation in binaries is concentrated in narrow rings where pressure gradients trap dust.
Misaligned and polar discs produce planets on inclined, eccentric, or retrograde orbits, and polar configurations around eccentric binaries offer a clear route to such planets.
Observational campaigns with ALMA, SPHERE, and future facilities should treat stellar multiplicity as a primary variable when interpreting disc structures, not as a contaminant.
Expanding the sample of imaged discs in multiples can convert current case studies into statistical links between orbital parameters and planetary architectures.

Reading between the lines

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

If the link between truncation and accelerated radial drift holds, binary discs should show a deficit of large grains relative to single-star discs at the same radius, a testable prediction for multiwavelength ALMA observations.
The same resonant-cavity physics should apply to circumtriple discs in higher-order systems, where the effective-binary approximation may mispredict cavity sizes and eccentricities; direct triple simulations could be compared with the GG Tau and GW Ori images.
The polar-alignment mechanism predicts that circumbinary planets on highly inclined orbits should preferentially orbit eccentric binaries, a demographic trend that future circumbinary-planet surveys can test.
Because the appendix sample is not statistically complete, a complete survey of discs in young binaries could either confirm or overturn the claimed frequencies of truncation and misalignment.

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Editorial analysis

A structured set of objections, weighed in public.

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

Desk Editor's Note

read the letter

Two things to know. First, this is a review, not a research paper; the only genuinely new content is a compiled catalogue of ~150 systems and a uniform re-reduction of archival ALMA/SPHERE images into a gallery. Second, the synthesis is competent and honest, but it leans heavily on the standard binary-torque cavity paradigm (Artymowicz & Lubow 1994 scaling) and never steps back to ask how often that paradigm actually works. The paper itself provides the counterexamples—UZ Tau E has a cavity at ≲0.08″ versus a predicted ~0.3″, and HD 142527's binary at ~11 au is too compact to explain its observed structures—and Section 5.1 concedes the binary-only scenario often fails. The authors present these as open questions, which is fair, but a reader coming to the field would not know whether the paradigm works for 10% or 80% of systems. That limits the strength of the conclusions about dust traps at cavity edges.

What the paper does well: the organization is logical (orbital parameters, CSDs, CBDs, dust, planet formation), the figures are useful, and the authors are careful to distinguish observed features from model interpretations. The compiled table and the uniform image processing are real added value for the community. The self-citations are numerous but used for specific modeling claims, not in a circular way.

Soft spots, in order of importance. The continuity equation (Eq. 1) is wrong as written: it is missing the v·∇ρ advection term, so even under the stated incompressible assumption it is not the correct continuity equation. In a review aimed at newcomers, that is a bad typo and should be fixed. The machine-readable table promised in Appendix B is not present in this version. And as noted above, the review would be substantially stronger if it quantified—even roughly—how often observed cavity sizes match the standard scalings.

Who is this for: graduate students and researchers entering the field, and anyone needing a current reference list of discs in multiples. It deserves a serious peer review, not because it advances the science, but because a competent review with a useful catalogue is worth publishing after fixes. My recommendation: engage with it, but the review should require the equation fix, the table, and preferably a short paragraph on the success/failure rate of the standard cavity scaling.

Referee Report

0 major / 6 minor

Summary. This review synthesizes observational and theoretical work on protoplanetary discs in multiple stellar systems, covering orbital characterization, circumstellar disc truncation and spirals, circumbinary disc cavities and alignment, dust dynamics, and implications for planet formation. It includes new archival SPHERE and ALMA images of ten systems and a table of dozens of known multiple systems with discs. The central claim is that stellar multiplicity is a first-order ingredient: it truncates discs, produces misalignment and polar configurations, and creates dust traps that shape planetary architectures.

Significance. The review is a useful, well-referenced synthesis of a fast-moving field, with concrete community value in its compilation of systems (Table B1) and its archival image gallery. It is careful to distinguish observed features from model interpretations and explicitly flags open questions. The main conclusions are consistent with the cited literature and are presented as a qualitative synthesis rather than as new quantitative predictions, so the central claim is credible. The manuscript's value would be enhanced by a slightly more careful treatment of the governing equations and a more explicit caveat about the statistical representativeness of the systems discussed.

minor comments (6)

[§2.2, Eq. (1)] The mass conservation equation ∂ρ/∂t + ρ(∇·v) = 0 is not the general continuity equation for a compressible gas; it should be ∂ρ/∂t + ∇·(ρv) = 0. The text also states that the fluid is assumed incompressible and follows an adiabatic equation of state, which is internally inconsistent because an adiabatic EOS implies compressibility. Please correct the equation or clarify the assumptions.
[§4.4, UZ Tau paragraph] The sentence 'the CBD shows only shows a small inner cavity of ≲ 0.08″' contains a duplicated 'shows'; this should be removed.
[§3.3] The statement that 'the precession rate varying as a3/2, where a is the radial distance' uses the symbol 'a' for radial distance, whereas 'a' is defined as the semi-major axis in Section 2.1; consider using 'r' to avoid confusion.
[§5.1] The discussion acknowledges systems where the binary scenario alone is insufficient (e.g., UZ Tau E, HD 142527, AB Aur), but the later synthesizing conclusions in Section 6 are stronger than this caveat warrants. An explicit sentence noting that the Table B1 sample is not statistically complete and that the simple resonant-truncation scaling is not universally applicable would temper the generalization appropriately.
[§4.1] The phrase 'with sizes scaling approximately with (1 + e)' is imprecise; the cavity size depends on binary separation and other parameters, and the eccentricity dependence is not simply linear. Please rephrase to avoid implying a direct proportionality to (1+e) alone.
[Appendix B, Table B1 caption] The caption states that the table 'will be available in a machine-readable format,' but no URL or deposition site is given; please specify where the machine-readable version will be hosted.

Circularity Check

0 steps flagged · score 0.0 of 10

Review is a synthesis of external observational and numerical results; no derivation chain reduces to its inputs.

full rationale

This is a review article, not a derivation or prediction paper. It contains no fitted parameters, no new equations used to produce predictions, and no uniqueness claim that is justified by the authors' own prior work. The central statements—e.g., that binaries truncate circumstellar discs and carve circumbinary cavities—are supported by citations to external surveys (DSHARP, ALMA surveys, SPHERE programs) and to independent hydrodynamical studies, and the review explicitly reports where the standard model fails (e.g., UZ Tau E shows only a ≲0.08″ cavity versus the ~0.3″ predicted by ref. [11]; HD 142527's ~11 au binary is 'insufficient to explain the observed features'). While the authors cite several of their own papers (e.g., refs. 16, 22, 27–29, 56, 62, 71, 79, 130, 134, 136, 162, 186, 187), those citations are used as representative field results, not to bootstrap a conclusion: the review's claims also rest on many external references, and no load-bearing step reduces by construction to a self-citation. There is therefore no circular step to exhibit.

Assumptions & free parameters 0 free parameters · 4 assumptions · 0 invented entities

The review introduces no free parameters, no new theoretical entities, and performs no fits. It relies on standard astrophysical background assumptions, listed above, which are all borrowed from the cited literature.

assumptions (4)

domain assumption Fluid description of protoplanetary discs via Navier-Stokes equations with artificial viscosity
Section 2.2 states that gas-dominated discs can be treated as fluids, which is standard in the field.
domain assumption Tidal truncation theory (Paczynski 1977; Artymowicz and Lubow 1994) gives the disc radius scaling
Section 3.1 relies on this to explain observed truncated disc sizes, and the HT Lup example uses the Miranda and Lai (2015) formula.
domain assumption Dust-gas coupling is characterized by the Stokes number and Epstein drag
Section 2.2 uses this to discuss radial drift and dust traps in Sections 5.2.
domain assumption Hydrodynamic simulations with simplified thermodynamics reproduce key binary-disc interaction features
Sections 5.1 and 5.3 compare simulations (e.g., refs 28, 29, 134) to observations, assuming their fidelity.

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Cite this review

Pith. "Pith review of Circumstellar and circumbinary discs in multiple stellar systems." pith.science (2026). https://pith.science/paper/GHOEEZ5A

@misc{pith2026250119249,
  author       = {Pith},
  title        = {Pith review of: Circumstellar and circumbinary discs in multiple stellar systems},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/GHOEEZ5A}},
  note         = {Machine review of arXiv:2501.19249}
}

read the original abstract

The interplay between stellar multiplicity and protoplanetary discs represents a cornerstone of modern astrophysics, offering key insights into the processes of planet formation. Protoplanetary discs act as cradles for planetary systems, yet their evolution and capacity to form planets are profoundly affected by gravitational forces within multiple stellar systems. This review synthesises recent advancements in observational and theoretical studies to explore the rich diversity of circumstellar and circumbinary discs within multiple stellar systems. We examine how stellar companions shape disc morphology through truncation, spirals, and misalignment. We also outline how dust dynamics and planetesimal formation are impacted by stellar multiplicity. On top of this, observations at high angular resolution reveal detailed disc structures, while simulations offer key insights into their evolution. Last, we consider the implications of stellar multiplicity for planetary system architectures, emphasising the diversity of planetary outcomes in such environments. Looking ahead, coordinated efforts combining high-resolution observations with advanced numerical models will be critical for unravelling the role of multiple stellar systems in shaping planetary formation and evolution.

Figures

Figures reproduced from arXiv: 2501.19249 by the authors.

**Figure 1.** Possible types of protoplanetary discs in systems with one star (left), two stars (centre), and three stars (right): circumstellar, circumbinary, or circumtriple. For simplicity, we show hierarchical stellar configurations only. For clarity, the circumstellar discs are shown in edge-on configurations. 2. Orbital parameters and typical disc parameters To describe stellar orbits alongside the dynamics and structure of… view at source ↗

**Figure 2.** Schematic illustration of the orbital parameters for an elliptical orbit: the inclination i, the argument of periapsis ω, the longitude of the ascending node Ω, and the true anomaly ν. Provided through the courtesy of Mario Sucerquia. The orbital parameters of multiple stellar systems can be precisely constrained through high-precision astrometric observations conducted over extended periods with instruments such as… view at source ↗

**Figure 3.** Gallery of observed circumstellar discs (CSDs) with external companions. Left column: ALMA 1.3 mm intensity maps (mJy/beam) with the synthesized beam and a 20 au scale bar (angular size noted). Right column: SPHERE polarized intensity data (% of peak value) processed with IRDAP, showing a 20 au scale bar and a green circle for the coronagraph position, if used. SPHERE data are at 1.65 µm, except 2.15 µm for HD 10045… view at source ↗

Figures from the paper (3 more)

**Figure 4.** Figure 4: Gallery of circumbinary discs (CBDs) with internal companions, processed using the same procedure as described in [PITH_FULL_IMAGE:figures/full_fig_p012_4.png]

**Figure 5.** Figure 5: Column density rendering of a hydrodynamical model of the system HD 100453 including a central star, a disc with an inner companion of 5 MJ at 20 au, and a misaligned external companion (star B) with the following parameters: q = 0.12, a = 207 au, e = 0.32, i = 49◦ , Ω…

**Figure 6.** Figure 6: Snapshots of three high-resolution simulations showing the gas density. Green dots represent the stars. The first column depicts the pure binary case, the central column shows a triple system obtained by splitting the secondary star of the binary (type ts), and the rig…

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Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

Dust Growth in Binary Systems: Inhibition of dust settling and growth in circumbinary discs
astro-ph.EP 2026-07 conditional novelty 5.0 of 10

Dust grains in circumbinary discs end up five times smaller than in single-star discs, and the conditions for streaming-instability clumping are not met, arguing against in-situ planet formation there.

Reference graph

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