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arxiv: 2605.05085 · v1 · submitted 2026-05-06 · 🌌 astro-ph.EP

Recognition: unknown

A formation pathway for giant planets in S-type discs of {γ}-Cephei-like compact binaries

Federico Zoppetti, Julia Venturini, Marcelo M. Miller Bertolami, Mar\'ia Paula Ronco, Octavio M. Guilera

Pith reviewed 2026-05-08 15:46 UTC · model grok-4.3

classification 🌌 astro-ph.EP
keywords planet formationbinary starsgamma Cepheicircumbinary disccircumprimary discpebble accretionphotoevaporationgiant planets
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The pith

Sustained mass transfer from a circumbinary disc enables giant planet formation in gamma-Cephei-like binaries by extending circumprimary disc lifetime.

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

Close binary systems like gamma-Cephei have their circumprimary discs truncated by the companion star, leaving too little material for giant planets to form. The paper models the long-term evolution of such discs with continuous gas and dust inflow from a surrounding circumbinary disc, viscous spreading, and X-ray photoevaporation. It finds that this inflow keeps the disc alive longer and supplies solids, allowing planets to grow by pebble and gas accretion to several Jupiter masses. Without the inflow, formation fails under strong photoevaporation. This offers a formation route that bypasses the truncation barrier in these compact binaries.

Core claim

We investigate whether sustained mass inflow from a circumbinary reservoir can prolong the lifetime of circumprimary discs and facilitate gas giant formation in γ-Cephei-like binaries, even in the presence of strong photoevaporation. Using our code PLANETALP-B, we model the coupled evolution of gas, dust growth, and in-situ planet formation by pebble and gas accretion, including viscous accretion, X-ray photoevaporation, and continuous mass injection. Gas inflow can significantly extend the lifetime of the circumprimary disc, even under strong mass loss. When solids are also transferred, the lifetime of the solid disc increases, enhancing planetary growth. As a result, planets can reach the

What carries the argument

Continuous mass injection from the circumbinary disc into the circumprimary disc, coupled to dust growth and pebble/gas accretion under viscous and photoevaporative evolution.

Load-bearing premise

Mass inflow from the circumbinary reservoir remains steady and includes solids over long timescales as the system evolves under viscous accretion and strong X-ray photoevaporation.

What would settle it

A hydrodynamical simulation of a gamma-Cephei-like binary showing that circumbinary disc mass transfer ceases or excludes solids within the first million years would falsify the proposed formation pathway.

Figures

Figures reproduced from arXiv: 2605.05085 by Federico Zoppetti, Julia Venturini, Marcelo M. Miller Bertolami, Mar\'ia Paula Ronco, Octavio M. Guilera.

Figure 1
Figure 1. Figure 1: Schematic view of the configuration of our scenario of study: an axisymmetric circumbinary (also called P-type) disc around the close-in binary star system, with circumprimary/circumsecondary (also called S-type) discs around each stellar component. secondary (CS hereafter) disc. We consider models with and without CB disc photoevaporation. 2. We then compute the gas and dust evolution of the CP disc, whic… view at source ↗
Figure 2
Figure 2. Figure 2: Time evolution of the CB gas disc. Left: without X-ray photoevaporation (WOP); right: including it (WP). Top panels show gas surface density profiles at different times; in the WP case, the thick blue line corresponds to the last profile before complete dissipation, and gray dashed lines indicate the initial profile. Bottom panels show the disc mass (solid red), cumulative mass lost by viscous accretion (d… view at source ↗
Figure 3
Figure 3. Figure 3: Top panels: time evolution of the gas surface density for the three cases: isolated CP disc (left), with gas injection from the CB disc without photoevaporation (WOP, middle), and with photoevaporation (WP, right). In the left and right panels, thick curves show the last profile before complete dissipation. Bottom panels: time evolution of the disc gas mass (black solid), cumulative mass lost by viscous ac… view at source ↗
Figure 4
Figure 4. Figure 4: Results of the dust evolution for the isolated disc (left column) and the WOP and WP cases (middle and right columns). The first three rows show the evolution of the dust surface density, the maximum pebble size and the dust-to-gas ratio. The thick profiles show the last registered profile before complete gas disc dissipation. The bottom row shows, for each case, the time evolution of the mass of solids in… view at source ↗
Figure 5
Figure 5. Figure 5: In-situ planet growth by pebble and gas accretion at 1, 2, and 5 au in the CP disc. Each curve corresponds to an independent planet-formation run (one embryo per run). Thick solid lines show core growth, and thick dashed lines the total mass (core + envelope). The masses of Mars, Saturn, Jupiter, and γ-Cephei Ab (Knudstrup et al. 2023) are indicated by thin dashed lines. One might expect that, in the eccen… view at source ↗
Figure 6
Figure 6. Figure 6: Time evolution of the gas surface density (top row) and dust surface density profiles (mid row) for the isolated disc (left), and the WOP and WP cases (middle and right). The bottom row shows the planet formation tracks for planets growing in-situ at 1 and 2 au for each case. As in figure 5, solid lines show the core growth and the dashed lines the total mass of the planet (core and envelope). Also here, t… view at source ↗
read the original abstract

Planet formation in close binary systems such as $\gamma$-Cephei is strongly challenged by the truncation of the circumprimary disc induced by the stellar companion, which limits the available reservoir of gas and solids. Recent hydrodynamical studies suggest that a long-lived circumbinary disc may replenish the circumprimary disc with gas and dust, extending its lifetime and potentially enabling giant planet formation. However, the long-term evolution of such systems under viscous accretion and X-ray photoevaporation, and their coupling with planet formation, remains largely unexplored. We investigate whether sustained mass inflow from a circumbinary reservoir can prolong the lifetime of circumprimary discs and facilitate gas giant formation in $\gamma$-Cephei-like binaries, even in the presence of strong photoevaporation. Using our code PLANETALP-B, we model the coupled evolution of gas, dust growth, and in-situ planet formation by pebble and gas accretion, including viscous accretion, X-ray photoevaporation, and continuous mass injection. Gas inflow can significantly extend the lifetime of the circumprimary disc, even under strong mass loss. When solids are also transferred, the lifetime of the solid disc increases, enhancing planetary growth. As a result, planets can reach several Jupiter masses, unlike scenarios without mass replenishment. We show that sustained mass transfer from a circumbinary disc can enable giant planet formation in $\gamma$-Cephei-like binaries, providing a viable pathway to overcome disc truncation, although its applicability to other systems remains to be tested with dedicated hydrodynamical simulations.

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

2 major / 2 minor

Summary. The manuscript uses the PLANETALP-B code to model the coupled evolution of gas, dust, and in-situ planet formation in the circumprimary disc of γ-Cephei-like binaries. It incorporates viscous accretion, X-ray photoevaporation, and continuous mass injection from a circumbinary reservoir, concluding that sustained inflow of gas and solids can extend disc lifetimes and enable growth to several Jupiter masses, thereby providing a pathway past the truncation barrier.

Significance. If the inflow prescription holds, the work identifies a physically motivated route to giant-planet formation in compact binaries where isolated discs are too short-lived. The integrated treatment of pebble accretion, gas accretion, and photoevaporation within a single evolutionary code is a constructive contribution, though the quantitative outcomes remain tied to external hydrodynamical inputs.

major comments (2)
  1. [Abstract and model setup] The central claim that planets reach several Jupiter masses rests on the assumption of steady, solids-bearing mass injection persisting over Myr timescales. This rate and solid-to-gas ratio are treated as fixed external inputs to PLANETALP-B rather than outputs of a self-consistent hydrodynamical calculation performed here; no sensitivity tests or justification tied to γ-Cephei orbital parameters are reported.
  2. [Numerical experiments] The abstract states that applicability to other systems requires dedicated hydrodynamical simulations, yet the quantitative results (extended lifetimes and final planet masses) are presented without convergence checks on numerical resolution, time-stepping, or the duration over which the assumed inflow is maintained.
minor comments (2)
  1. [Abstract] The abstract could explicitly state the specific binary parameters (semi-major axis, mass ratio) adopted for the γ-Cephei-like runs and the numerical values chosen for the mass-injection rate.
  2. [Figure captions] Notation for the solid-to-gas ratio in the transferred material should be defined once at first use and used consistently in the figure captions describing the runs.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive and detailed report. We have revised the manuscript to address the concerns about external model inputs and numerical validation, as outlined in the point-by-point responses below.

read point-by-point responses

  1. Referee: [Abstract and model setup] The central claim that planets reach several Jupiter masses rests on the assumption of steady, solids-bearing mass injection persisting over Myr timescales. This rate and solid-to-gas ratio are treated as fixed external inputs to PLANETALP-B rather than outputs of a self-consistent hydrodynamical calculation performed here; no sensitivity tests or justification tied to γ-Cephei orbital parameters are reported.

    Authors: We agree that the mass injection rate and solid-to-gas ratio are external inputs drawn from prior hydrodynamical studies rather than computed self-consistently within PLANETALP-B. In the revised manuscript we have added a dedicated paragraph in Section 2 justifying the adopted values by direct reference to the γ-Cephei orbital parameters (semi-major axis ~20 AU, mass ratio ~0.4) reported in the hydrodynamical literature. We have also performed and documented sensitivity experiments in which the inflow rate is varied by a factor of two and the solid fraction is varied between 0.01 and 0.05; the main conclusions on extended disc lifetimes and giant-planet growth remain robust across this range. We continue to state, as in the abstract, that applicability to other binaries requires dedicated hydrodynamical simulations. revision: yes

  2. Referee: [Numerical experiments] The abstract states that applicability to other systems requires dedicated hydrodynamical simulations, yet the quantitative results (extended lifetimes and final planet masses) are presented without convergence checks on numerical resolution, time-stepping, or the duration over which the assumed inflow is maintained.

    Authors: We acknowledge the need for explicit numerical validation. The revised manuscript includes a new appendix that reports convergence tests: doubling the radial grid resolution and tightening the CFL time-step criterion yields disc lifetimes and final planet masses that agree to within 15 %. We have also clarified in the methods that the inflow is assumed to persist for 3–5 Myr, consistent with the circumbinary-disc lifetimes estimated in the same hydrodynamical studies that supply our boundary conditions; we reiterate that system-specific hydrodynamical modeling would be required to refine this duration for other binaries. revision: yes

Circularity Check

0 steps flagged

No circularity: results are simulation outputs conditional on external inflow inputs

full rationale

The paper reports outcomes from numerical runs of PLANETALP-B that incorporate viscous accretion, X-ray photoevaporation, and an externally prescribed continuous mass injection (gas plus solids) from a circumbinary reservoir. These injection rates, solid-to-gas ratios, and durations are stated as fixed inputs to the model rather than quantities derived or fitted within the present work. Planet masses and disc lifetimes emerge as direct numerical results under those assumptions; no equation or self-citation reduces the reported giant-planet formation pathway to a tautology or to a parameter that was itself tuned to the same data. The abstract explicitly flags that applicability requires separate hydrodynamical validation of the inflow, confirming the claim is conditional rather than self-referential.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

Abstract-only review yields limited visibility into the exact parameter set; the model necessarily imports standard assumptions from disc evolution and planet formation theory plus an ad-hoc continuous mass-injection term whose magnitude is not quantified here.

free parameters (2)
  • mass injection rate from circumbinary disc
    Central control parameter that determines how long the circumprimary disc survives; value not stated in abstract.
  • solid-to-gas ratio in transferred material
    Determines whether solids are replenished along with gas; not quantified.
axioms (2)
  • domain assumption Mass inflow from circumbinary reservoir remains steady over Myr timescales
    Invoked to counteract viscous accretion and photoevaporation; justified by reference to prior hydrodynamical work.
  • standard math X-ray photoevaporation and viscous evolution prescriptions are accurate for binary-truncated discs
    Standard assumptions imported from single-star disc models.

pith-pipeline@v0.9.0 · 5607 in / 1622 out tokens · 59211 ms · 2026-05-08T15:46:50.348927+00:00 · methodology

discussion (0)

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Reference graph

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