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arxiv: 2601.00741 · v2 · submitted 2026-01-02 · 🌌 astro-ph.HE · astro-ph.GA

Recognition: 2 theorem links

· Lean Theorem

Eccentric Disks from Gaseous Rings around Equal-Mass, Circular Binaries

Leonardo Betancourt , Andrew MacFadyen , Jonathan Zrake
Authors on Pith no claims yet

Pith reviewed 2026-05-16 17:53 UTC · model grok-4.3

classification 🌌 astro-ph.HE astro-ph.GA
keywords circumbinary diskseccentric disksgaseous ringsbinary accretionstream impactquasi-periodic eruptionshydrodynamics simulationsblack hole binaries
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The pith

Gaseous rings around equal-mass circular binaries evolve into eccentric disks that suppress accretion when cold.

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

The paper performs high-resolution hydrodynamics simulations of gaseous rings viscously spreading into disks around equal-mass circular binaries. It finds that cold compact rings develop high eccentricity up to 0.7 through a stream impact process and that accretion onto the binary is suppressed in all cold cases. Variability shows a dominant peak at roughly 0.1 times the binary orbital frequency. These results matter because they offer a pathway to explain quasi-periodic eruptions from intermediate-mass black hole binaries and asymmetric time-variable line emission in galactic nuclei disks. The work concludes that any binary-driven asymmetry in line profiles would require a very compact initial ring.

Core claim

High-resolution grid-based hydrodynamics simulations of gaseous rings around equal-mass circular binaries show that all cold systems suppress accretion. Eccentricity grows strongly depending on initial ring radius and gas temperature, reaching values near 0.7 for smaller colder rings with nearly radius-independent profiles that persist out to several times the initial semimajor axis. Eccentricity growth is attributed to a stream impact mechanism in which gas torqued by the binary at pericenter passage exerts a perturbative force on the cavity wall. The configuration is considered for inefficiently accreting intermediate-mass black hole binaries as sources of quasi-periodic eruptions when the

What carries the argument

Stream impact mechanism in which gas torqued by the binary at pericenter passage exerts a perturbative force on the cavity wall to drive eccentricity growth.

If this is right

  • Accretion onto the binary is suppressed in relatively cold gas.
  • Eccentricity reaches up to 0.7 for smaller colder rings and remains high out to several times the initial semimajor axis.
  • Dominant spectral variability appears at approximately 0.1 times the binary orbital frequency.
  • Rejected streams can shock the cavity wall and radiate in the UV or soft X-ray for intermediate-mass black hole binaries.
  • Binary-driven asymmetry in accretion disk line profiles requires a very compact progenitor circumbinary ring.

Where Pith is reading between the lines

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

  • Observed flat eccentricity profiles extending to large radii in circumbinary disks would support stream impact as the dominant driver over other torques.
  • The strong temperature dependence implies that self-consistent heating from shocks could regulate eccentricity growth in more realistic models.
  • Similar eccentricity development might appear in stellar binary systems with protoplanetary disks under comparable cold compact conditions.
  • Eccentric disks formed this way could alter gas-driven migration rates for embedded planets or affect electromagnetic signatures around merging binaries.

Load-bearing premise

The gas is relatively cold and the initial ring is compact.

What would settle it

A simulation or observation showing a warm or spatially extended initial ring developing eccentricity above 0.5 without stream impacts would falsify the mechanism.

Figures

Figures reproduced from arXiv: 2601.00741 by Andrew MacFadyen, Jonathan Zrake, Leonardo Betancourt.

Figure 1
Figure 1. Figure 1: (Top) Accretion rate timeseries of the infinite disk in quasi-steady-state, normalized by the large-scale inflow rate, M˙ ∞ = 3πΣ0νa¯ 2Ωb. (Bottom) Accretion rate timeseries of the R0 = 4a ring well after tvisc. In both plots, the dashed lines represent the time-averaged normalized accretion rates. −100 −10−1 0 10−1 100 (˙a/ ˙ M)accr [a/M] M = 10 M = 60 −104 −102 0 102 104 (˙a/ ˙ M)grav [a/M] 2600 2650 270… view at source ↗
Figure 2
Figure 2. Figure 2: Accretion (top), gravity (middle), and total (bot￾tom) contributions to the time-derivative of the binary semi￾major axis a. infinite disk, where the M = 60 disk accretes at a rate ∼ 10% of the M = 10 disk. The time-averaged accre￾tion rates decrease monotonically with increasing M. The bottom panel shows a very similar suppression fac￾tor in the relaxed ring of relatively cold (M = 60) gas. This suggests … view at source ↗
Figure 3
Figure 3. Figure 3: 100-orbit windows of the accretion rate (top) and the corresponding Lomb-Scargle periodogram (bottom) computed over 100 orbits in quasi-steady-state. Left and right panels compare ring and infinite disk initial conditions (ICs) respectively [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Eccentricity e = [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: (Top) Density snapshots of ring R0 = 2a and M = {10, 60} at similar phases of precession. (Bottom) Corresponding velocity line profiles along the line of sight (LOS) chosen along the positive x-direction. et al. 2003) and from disks evolved from TDEs (Wevers et al. 2022). In the latter, the extreme eccentricity of the disk (e = 0.91±0.01) allows for measurement of the time-evolution of the double-peaks dur… view at source ↗
read the original abstract

We perform high-resolution, grid-based hydrodynamics simulations of gaseous rings viscously spreading into disks around equal-mass, circular binaries. We find that all systems suppress accretion onto the binary when the gas is relatively cold. Circumbinary rings (CBRs) display weak variability above the binary orbital frequency $\Omega_b$ and a dominant spectral peak at $\sim0.1\Omega_b$ (half the fiducial lump frequency of $\sim0.2\Omega_b$). The evolution of CBR eccentricity depends strongly on both the initial ring radius and gas temperature, with smaller, colder rings exhibiting higher eccentricity up to $e \simeq 0.7$. Cold, compact rings develop nearly radius-independent eccentricity profiles, maintaining large $e$ out to several times the initial gas semimajor axis. We find that eccentricity growth favors a stream impact mechanism, in which gas torqued by the binary at pericenter passage exerts a perturbative force on the cavity wall. We consider inefficiently-accreting, intermediate-mass ($\sim10^4 M_\odot$) black hole binaries as sources of quasi-periodic eruptions when rejected streams shock the cavity wall and radiate in the UV or soft X-ray. We discuss the implications of eccentric disks evolved from CBRs for quasar light curves and asymmetric, time-variable double-peaked line emission from disks in galactic nuclei. If binaries drive asymmetry in accretion disk line profiles, our study suggests that the progenitor CBR must have been very compact.

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 reports high-resolution grid-based hydrodynamics simulations of viscously spreading gaseous rings forming circumbinary disks around equal-mass circular binaries. Key results include accretion suppression for relatively cold gas, weak variability above the binary orbital frequency Ω_b with a dominant spectral peak at ~0.1 Ω_b, and strong dependence of disk eccentricity evolution on initial ring radius and gas temperature, with smaller colder rings reaching e ≃ 0.7 and developing nearly radius-independent eccentricity profiles. Eccentricity growth is attributed to a stream impact mechanism in which gas torqued by the binary at pericenter exerts force on the cavity wall. Implications are discussed for quasi-periodic eruptions from inefficiently accreting ~10^4 M_⊙ black hole binaries and for asymmetric time-variable line emission in quasar disks, requiring compact progenitor rings.

Significance. If the numerical results hold, the work provides direct evidence for eccentricity excitation in circumbinary disks originating from initial rings, with a proposed physical mechanism tied to stream impacts. This has potential to explain observed variability in AGN light curves and double-peaked lines, as well as QPEs in intermediate-mass binaries. The parameter exploration of initial ring radius and temperature, combined with direct integration of the hydrodynamic equations without fitted parameters, strengthens the findings and underscores the sensitivity of outcomes to realistic initial conditions.

major comments (1)
  1. [Abstract and Results] Abstract and results on eccentricity: The claim that eccentricity growth favors the stream impact mechanism is demonstrated only in the regime of small, cold initial rings that achieve high eccentricity (e ≃ 0.7). For warmer or larger rings where eccentricity remains low, the manuscript does not demonstrate that stream impact dominates other torques, rendering the initial-condition dependence load-bearing for the favored-mechanism conclusion.
minor comments (3)
  1. [Abstract] The abstract states that cold compact rings develop nearly radius-independent eccentricity profiles; specify the section or figure where this is quantified and shown across radii.
  2. [Introduction] Add references to prior circumbinary disk studies on lump frequencies (~0.2 Ω_b) to contextualize the reported ~0.1 Ω_b peak.
  3. [Figures] Ensure figures clearly label the parameter variations in initial ring radius and gas temperature used in the eccentricity evolution plots.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their thorough review and positive assessment of our work on eccentric disks from gaseous rings around binaries. We address the major comment on the eccentricity mechanism below and have revised the manuscript to provide additional clarification and analysis.

read point-by-point responses

  1. Referee: [Abstract and Results] Abstract and results on eccentricity: The claim that eccentricity growth favors the stream impact mechanism is demonstrated only in the regime of small, cold initial rings that achieve high eccentricity (e ≃ 0.7). For warmer or larger rings where eccentricity remains low, the manuscript does not demonstrate that stream impact dominates other torques, rendering the initial-condition dependence load-bearing for the favored-mechanism conclusion.

    Authors: We agree that the demonstration of the stream impact mechanism is most direct in the high-eccentricity regime achieved by small, cold rings. In the low-eccentricity cases for warmer or larger rings, the net eccentricity growth is indeed smaller, but our torque calculations indicate that the stream impact still provides the leading contribution to eccentricity excitation, with other torques (such as those from the binary's gravitational potential) being either opposing or less effective in driving net growth. To make this explicit, we have added a new panel to Figure 8 showing the time-averaged torque contributions from stream impacts versus other sources for representative low-e and high-e runs. We have also revised the abstract to read 'eccentricity growth favors a stream impact mechanism, particularly in compact, cold rings' and expanded the discussion section to address the initial-condition dependence. These changes clarify the scope of our claims while preserving the overall conclusions. revision: yes

Circularity Check

0 steps flagged

No circularity: results are direct outputs of hydrodynamic simulations

full rationale

The paper reports outcomes from grid-based hydrodynamics simulations of viscous spreading of gaseous rings into circumbinary disks. Central claims (eccentricity growth up to e ≃ 0.7 for cold compact rings, dominance of stream-impact torques, suppression of accretion) are stated as findings from the numerical integrations themselves, with explicit dependence on initial ring radius and temperature reported as a result rather than a hidden premise. No equations, fitted parameters, or self-citations are shown that reduce the reported mechanism or profiles back to the inputs by construction. The study is therefore self-contained; the initial-condition sensitivity is a disclosed limitation, not a circular justification.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

The central claims rest on choices of initial ring radius and gas temperature as explored parameters, plus standard assumptions of viscous hydrodynamics in astrophysical disks.

free parameters (2)
  • initial ring radius
    Varied across simulations; smaller values produce higher eccentricity up to 0.7 and radius-independent profiles.
  • gas temperature
    Determines cold regime where accretion is suppressed and eccentricity grows; warmer gas yields different behavior.
axioms (1)
  • standard math Gas evolution follows standard viscous hydrodynamic equations on a grid
    Core assumption of all grid-based hydrodynamics simulations for astrophysical disks.

pith-pipeline@v0.9.0 · 5572 in / 1309 out tokens · 49103 ms · 2026-05-16T17:53:03.664459+00:00 · methodology

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