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arxiv: 2605.19241 · v1 · pith:HOYIWCOCnew · submitted 2026-05-19 · 🌌 astro-ph.EP · astro-ph.GA· astro-ph.HE· astro-ph.SR

Active Galactic Nucleus Tori: Potential Birthplace to Millions of Planets

Bhupendra Mishra , Wladimir Lyra , Barry McKernan , Mordecai-Mark Mac Low , K. E. Saavik Ford , Harrison E. Cook This is my paper

Pith reviewed 2026-05-20 03:20 UTC · model grok-4.3

classification 🌌 astro-ph.EP astro-ph.GAastro-ph.HEastro-ph.SR
keywords active galactic nucleidust toriplanet formationstreaming instabilitypebble accretionplanetesimalscore accretion
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The pith

AGN dust tori can form tens of millions of planets via streaming instability.

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

The paper argues that the outer regions of active galactic nucleus disks reach temperatures similar to those around young stars, allowing dust to condense and grow. Using a strongly magnetized disk model that prevents gravitational collapse, dust particles coagulate until they trigger streaming instability, forming dense filaments that hold solar masses of material. These filaments fragment into tens of millions of planetesimals with masses from Earth-like to super-Jupiter sizes. The resulting objects accrete pebbles and gas on short timescales, sometimes reaching stellar masses through a core-accretion pathway before feedback halts growth, leading the authors to conclude that AGN tori contain the largest planetary populations anywhere.

Core claim

In AGN dust tori, dust grains coagulate to sizes enabling streaming instability, producing filaments of solar mass that fragment into tens of millions of planetesimals ranging from Earth to super-Jupiter masses. These bodies typically form in the 3D Bondi regime of pebble accretion with mass-doubling times between 10^3 and 10^7 years, and can undergo concurrent gas accretion to reach crossover mass. The pebble isolation mass exceeds the hydrogen burning limit, allowing growth to stellar masses limited by feedback rather than gap opening, and the model also predicts pure-dust objects formed directly above that limit.

What carries the argument

Streaming instability triggered by coagulated dust in a magnetized, gravitationally stable AGN disk model, forming filaments that collapse into planetesimals followed by pebble and gas accretion.

If this is right

  • Coagulation readily produces the dust grain sizes required to trigger streaming instability.
  • Dust filaments contain solar masses and collapse into tens of millions of planetesimals spanning Earth to super-Jupiter masses.
  • Planets form mainly in the 3D Bondi regime of pebble accretion with mass-doubling times from 10^3 to 10^7 years.
  • Gas accretion proceeds to crossover mass and can produce stellar-mass objects, creating a core-accretion channel for star formation.
  • Growth is limited by stellar feedback because the pebble isolation mass lies above the hydrogen-burning limit.

Where Pith is reading between the lines

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

  • If correct, AGN tori would represent a previously unrecognized dominant site of planet formation that could dominate the cosmic census of planets.
  • The rapid formation of many massive bodies might alter the long-term structure and stability of AGN disks through dynamical interactions.
  • Signatures of embedded planets or unusual dust evolution in AGN observations could provide a direct test of the predicted timescales.

Load-bearing premise

The outer regions of AGN disks have temperatures low enough for dust to condense like in circumstellar disks, and a strongly magnetized disk model keeps the structure gravitationally stable.

What would settle it

A direct measurement of outer AGN disk temperatures above the dust condensation threshold or grain sizes remaining below the threshold for streaming instability would show the process cannot occur.

Figures

Figures reproduced from arXiv: 2605.19241 by Barry McKernan, Bhupendra Mishra, Harrison E. Cook, K. E. Saavik Ford, Mordecai-Mark Mac Low, Wladimir Lyra.

Figure 1
Figure 1. Figure 1: Radial disk profiles of relevant quantities for an AGN disk with three different central SMBH masses 𝑀SMBH = 109 , 108 , and 107 𝑀⊙ (following the legend), and magnetic plasma 𝛽𝑚 = 0.01. The viscosity parameter is fixed to 𝛼 = 10−4 to define the mass accretion rate; the hydrogen abundance in the disk is 𝑋 = 0.7. The top row shows density (𝜌) and temperature (𝑇). The second row shows surface density (𝛴) and… view at source ↗
Figure 2
Figure 2. Figure 2: Streaming instability parameters based on the AGN disk profile shown in [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Similar to Fig. 2a, 2b and 2d but for 𝑣frag = 10 m s−1 (top panel) and 𝑣frag = 1 m s−1 and StSI = 10−3 (bottom panel). 2.4. Characteristic planetesimal mass The dust in the filament will collapse gravitationally and produce planets if it reaches Roche density 𝜌Roche ≡ 9𝛺 2 4𝜋𝐺 . (20) The filament mass will not produce a single planet, but will instead fragment into many objects, with a characteristic size … view at source ↗
Figure 4
Figure 4. Figure 4: Transition between different accretion regimes as shown by the shading and top labels. From left to right the panels show central AGN masses of 109 , 108 and 107 𝑀⊙. The top row shows 𝑣frag = 1 m s−1 and the bottom row shows 𝑣frag = 10 m s−1 . The symbol 𝑚p gives the characteristic planetesimal mass, 𝑀HB is the transition mass between the Hill and the Bondi accretion regime, 𝑀BG is the transition mass betw… view at source ↗
Figure 5
Figure 5. Figure 5: The e-folding growth time for the planets given the planetesimal mass at formation and pebble accretion rate. The top row shows 𝑣frag = 1 m s−1 and the bottom row 𝑣frag = 10 m s−1 . 10 1 10 0 10 1 10 2 R[pc] 10 2 10 3 10 4 10 5 Total Number of Filaments Mbh = 10 9 M Mbh = 10 8 M Mbh = 10 7 M 10 1 10 0 10 1 10 2 R[pc] 10 4 10 5 10 6 Total Number of Planets Mbh = 10 9 M Mbh = 10 8 M Mbh = 10 7 M [PITH_FULL_… view at source ↗
Figure 6
Figure 6. Figure 6: Cumulative sum over radius of number of filaments (left) and total number of planets (right) [PITH_FULL_IMAGE:figures/full_fig_p012_6.png] view at source ↗
read the original abstract

The outer regions of AGN disks have temperatures similar to those of circumstellar disks, permitting dust condensation. Therefore, planet formation and growth could be active in these dust tori through similar mechanisms. We aim at quantifying the parameter space for the occurrence of streaming instability, and its outcomes in terms of the masses of the objects formed, their total number, and their continued growth via pebble accretion. We use a a recently proposed disk model with strong magnetization to keep the disk gravitationally stable. We find that the dust grain sizes required for streaming instability are easily attained through coagulation; the dust filaments it produces can contain solar masses, collapsing into tens of millions of planetesimals ranging from Earth to super-Jupiter masses. These planets are usually born in the 3D Bondi regime of pebble accretion, and have mass-doubling times from 10^3 to 10^7 yrs, though 3D Hill and geometric accretion are also realized. Gas accretion occurs concurrently, and crossover mass can be attained while still in the planetary mass range. As a result, vigorous accretion can occur, leading to objects with stellar masses -- defining a core accretion channel for star formation. The pebble isolation mass is beyond the hydrogen burning limit, so accretion is limited by stellar feedback instead of gap carving. Our model also predicts a population of exotic objects directly formed above the hydrogen burning limit, yet of pure dust. Our approximate model suggests that AGN dust tori host the largest populations of planets in the universe.

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 claims that the outer regions of AGN dust tori have temperatures similar to circumstellar disks, enabling dust condensation and planet formation via streaming instability. Using a recently proposed strongly magnetized disk model to ensure gravitational stability, the authors estimate that dust filaments contain solar masses and collapse into tens of millions of planetesimals (Earth to super-Jupiter masses). These objects grow via pebble accretion (primarily in the 3D Bondi regime) with mass-doubling times of 10^3–10^7 yr, concurrent gas accretion can reach crossover mass, and the pebble isolation mass exceeds the hydrogen-burning limit, so stellar feedback limits growth instead of gap carving. The model also predicts exotic pure-dust objects formed above the hydrogen-burning limit and concludes that AGN tori host the largest planetary populations in the universe.

Significance. If the temperature and stability assumptions hold, the work identifies a previously unrecognized channel for both planet and star formation in AGN environments, with quantitative predictions for planetesimal numbers, accretion timescales, and exotic objects that could be tested observationally. It would substantially expand the parameter space of known planet-forming sites and link core accretion to stellar-mass outcomes.

major comments (2)
  1. [Methods and model choice] The load-bearing assumption that outer AGN tori reach T ~ 100–300 K (permitting dust condensation) and remain Toomre-stable via the adopted strongly magnetized disk model is stated in the abstract and methods paragraph but is not validated against standard AGN radiative-transfer calculations or observed B-field strengths at large radii. If AGN heating raises T or weaker magnetization yields Q < 1, the streaming-instability channel collapses; a direct comparison or sensitivity test is required.
  2. [Results on streaming instability and planetesimal formation] The quantitative outcomes (solar-mass filaments, tens of millions of planetesimals, mass-doubling times 10^3–10^7 yr, crossover while still planetary) are presented in the results section without explicit equations, adopted parameter values, or verification that the numbers reduce independently of the external disk model rather than being inherited from it.
minor comments (2)
  1. [Abstract] Abstract contains a typographical error: 'We use a a recently proposed' should read 'We use a recently proposed'.
  2. [Abstract and conclusions] The strong concluding claim that AGN tori host 'the largest populations of planets in the universe' would be strengthened by a brief quantitative comparison to the total planet inventory expected from circumstellar disks or galactic-field populations.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive review and recommendation for major revision. We address the two major comments point by point below, agreeing to incorporate additional validations and explicit derivations in the revised manuscript.

read point-by-point responses

  1. Referee: [Methods and model choice] The load-bearing assumption that outer AGN tori reach T ~ 100–300 K (permitting dust condensation) and remain Toomre-stable via the adopted strongly magnetized disk model is stated in the abstract and methods paragraph but is not validated against standard AGN radiative-transfer calculations or observed B-field strengths at large radii. If AGN heating raises T or weaker magnetization yields Q < 1, the streaming-instability channel collapses; a direct comparison or sensitivity test is required.

    Authors: We agree that further validation strengthens the central assumptions. The adopted temperature range follows from the outer tori being shielded from intense central radiation in standard AGN disk models, and the strongly magnetized framework is taken from the recently proposed model referenced in the manuscript to ensure Q > 1. To address the comment directly, we will add a dedicated methods subsection that compares our T and magnetization values against published radiative-transfer calculations for AGN disks and discusses available constraints on B-field strengths at large radii from observations. We will also include a brief sensitivity test varying T by factors of two and magnetization strength to show the robustness of the streaming instability regime. These additions will appear in the revised version. revision: yes

  2. Referee: [Results on streaming instability and planetesimal formation] The quantitative outcomes (solar-mass filaments, tens of millions of planetesimals, mass-doubling times 10^3–10^7 yr, crossover while still planetary) are presented in the results section without explicit equations, adopted parameter values, or verification that the numbers reduce independently of the external disk model rather than being inherited from it.

    Authors: We acknowledge that the results would be clearer with explicit derivations. The quoted quantities are obtained by applying standard streaming-instability thresholds (critical dust-to-gas ratio and stopping time) and pebble-accretion rate formulas to the local surface density, temperature, and dust properties supplied by the magnetized disk model. Filament mass follows from the most unstable wavelength, planetesimal count from total dust mass divided by characteristic planetesimal mass, and doubling times from the 3D Bondi regime expression. In the revision we will insert an expanded methods or appendix section containing the governing equations, a table of all adopted numerical values (e.g., dust fraction, grain size, viscosity parameter), and a short demonstration that the outcomes scale directly with the local disk quantities rather than depending on global model details beyond those quantities. This will make the calculations fully reproducible. revision: yes

Circularity Check

0 steps flagged

No significant circularity; derivation applies standard mechanisms to externally adopted disk conditions.

full rationale

The paper adopts temperatures and gravitational stability from a recently proposed external disk model with strong magnetization, then applies standard streaming instability, coagulation, pebble accretion, and core accretion calculations to those conditions. No equations or results within the paper reduce by construction to fitted inputs, self-definitions, or load-bearing self-citations that lack independent verification. The central claim follows from mapping known planet-formation physics onto the AGN torus parameter space under the stated assumptions, remaining self-contained against external benchmarks for those processes.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

Abstract-only review limits identification of exact parameters; the work rests on an external disk model whose magnetization strength and stability assumptions are not detailed here.

free parameters (1)
  • magnetization strength in disk model
    Used to keep the disk gravitationally stable; value not specified in abstract but central to the setup.
axioms (1)
  • domain assumption Outer AGN disk regions have temperatures similar to circumstellar disks, permitting dust condensation
    Stated directly in the abstract as the basis for applying circumstellar formation mechanisms.

pith-pipeline@v0.9.0 · 5838 in / 1448 out tokens · 40571 ms · 2026-05-20T03:20:00.163415+00:00 · methodology

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