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arxiv: 2606.28293 · v1 · pith:MLYRUJ7Onew · submitted 2026-06-26 · 🌌 astro-ph.HE · astro-ph.GA

Accretion-Driven Evolution of Compact-Object Populations in Gas-Rich Environments and the Origin of Massive Gravitational-Wave Sources

Mor Rozner , Alejandra Rosselli-Calderon , Enrico Ramirez-Ruiz This is my paper

Pith reviewed 2026-06-29 02:36 UTC · model grok-4.3

classification 🌌 astro-ph.HE astro-ph.GA
keywords accretioncompact objectsgravitational wavesmass distributionbinary evolutioncontinuity equationgas-rich environmentshigh-mass black holes
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The pith

Gas accretion acts as mass-space transport that broadens compact-object distributions when the accretion rate scales steeper than linearly with mass.

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

The paper treats sustained gas accretion onto compact objects as a transport process governed by a continuity equation in mass space. Population evolution is controlled by the exponent β in the accretion-rate scaling ˙m ∝ m^β. Laws with β greater than one drive divergent evolution that stretches distributions into high-mass tails, while β less than one produces convergent evolution that narrows the range. Applied to binaries, collective accretion pushes mass ratios toward equality. The framework supplies a pathway for populating the high-mass end of gravitational-wave catalogs in gas-rich settings.

Core claim

Using a continuity-equation framework, we demonstrate that population evolution is governed primarily by the mass dependence of the accretion rate, ˙m ∝ m^β. Accretion laws with β>1 naturally produce divergent evolution and generate extended high-mass tails, whereas β<1 leads to convergent evolution and compresses the population toward a narrower range of masses. We show that sustained gas accretion can substantially broaden compact-object mass distributions, populate the high-mass end of gravitational-wave catalogs, and alter the mass-ratio distribution of compact-object binaries. In particular, collective accretion within compact binaries drives their mass ratios toward unity.

What carries the argument

Continuity-equation framework in which accretion rate scaling ˙m ∝ m^β determines whether populations diverge into high-mass tails or converge to a narrow mass range.

If this is right

  • Accretion laws with β>1 generate extended high-mass tails in compact-object populations.
  • Collective accretion in binaries drives mass ratios toward unity.
  • Massive gravitational-wave events such as GW231123 become reachable through sustained accretion.
  • Gravitational-wave catalogs exhibit broader mass distributions when gas-rich environments are common.

Where Pith is reading between the lines

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

  • The same transport process could reshape mass distributions in other accreting systems where β exceeds one.
  • Environmental dependence of mass distributions could be tested by comparing field versus cluster populations.
  • If β is measured from individual accretion events, the model predicts observable shifts in binary mass-ratio histograms over time.

Load-bearing premise

The population evolution is governed primarily by the mass dependence of the accretion rate without other processes such as dynamical interactions or mergers dominating in gas-rich environments.

What would settle it

A survey of compact-object masses in gas-rich galaxies that shows neither extended high-mass tails nor a preference for equal-mass binaries would falsify the predicted transport effect.

Figures

Figures reproduced from arXiv: 2606.28293 by Alejandra Rosselli-Calderon, Enrico Ramirez-Ruiz, Mor Rozner.

Figure 1
Figure 1. Figure 1: illustrates the trajectories of compact ob￾jects in a representative AGN-disk environment, where growth is regulated by the Hill accretion prescription. Even in this convergent regime (β = 2/3), more massive objects evolve more rapidly than lower-mass objects, providing a concrete example of the differential growth discussed in Section 2. These trajectories foreshadow how accretion-driven transport reshape… view at source ↗
Figure 2
Figure 2. Figure 2: Evolution of the normalized primary-mass dis￾tribution under sustained gas accretion. The initial popula￾tion consists of a Salpeter-like power law combined with a Gaussian component centered at µ = 10 M⊙, with masses drawn between 5 and 50 M⊙. The gas density evolves as ρg(t) = 7 × 10−16 exp(−t/τgas) g cm−3 with τgas = 10 Myr. Different colors show the mass function at successive times. Solid curves corre… view at source ↗
Figure 3
Figure 3. Figure 3: Time evolution of binary populations in the absence of secondary accretion enhancement, i.e. m˙ 2 = q 2 /(1 + q) 2M, ˙ m˙ 1 = (1 + 2q)/(1 + q) 2 , m2 accretes as isolated and m1 completes to the total expected common accretion rate, according to the relevant regime. The calculations are based on Monte Carlo simulations with 5 × 106 realiza￾tions, assuming an initial gas density of ρg,0 = 10−18g cm−3 and a … view at source ↗
Figure 4
Figure 4. Figure 4: Time evolution of binary populations including enhanced accretion onto the secondary companion. The calculations are identical to those shown in [PITH_FULL_IMAGE:figures/full_fig_p008_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Probability distribution of the gravitational-wave merger rate as a function of primary mass. The distributions are derived from the evolving compact-object populations shown in previous sections and therefore represent the observable consequences of accretion-driven transport through mass space. Top Left: evolution of a fully accreting population, illustrating the progressive development of a high-mass me… view at source ↗
read the original abstract

The origin of the most massive gravitational-wave sources remains elusive. We show that gas accretion can be understood as a transport process in mass space, causing compact objects to migrate through a population at rates determined by the underlying growth law. Using a continuity-equation framework, we demonstrate that population evolution is governed primarily by the mass dependence of the accretion rate, $\dot m \propto m^\beta$. Accretion laws with $\beta>1$ naturally produce divergent evolution and generate extended high-mass tails, whereas $\beta<1$ leads to convergent evolution and compresses the population toward a narrower range of masses. We apply this framework to physically motivated accretion regimes and explore their consequences using analytical calculations and Monte Carlo population models. We show that sustained gas accretion can substantially broaden compact-object mass distributions, populate the high-mass end of gravitational-wave catalogs, and alter the mass-ratio distribution of compact-object binaries. In particular, collective accretion within compact binaries drives their mass ratios toward unity. Our results suggest that gaseous environments act as transport media that continuously reshape compact-object populations, providing a natural pathway toward the formation of massive mergers such as GW231123 and the high-mass tails increasingly revealed by gravitational-wave observations.

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 / 1 minor

Summary. The manuscript applies a continuity-equation framework to compact-object population evolution under gas accretion, with accretion rate scaling as \dot{m} o m^eta. It claims that eta > 1 produces divergent evolution and high-mass tails while eta < 1 produces convergent evolution; sustained accretion thereby broadens mass distributions, populates the high-mass end of gravitational-wave catalogs, and drives binary mass ratios toward unity via collective accretion within binaries.

Significance. If the central results hold, the work supplies a general transport-process description of how gaseous environments can reshape compact-object mass and mass-ratio distributions, offering a pathway to the high-mass gravitational-wave events (e.g., GW231123) that is complementary to purely dynamical channels.

major comments (2)
  1. [Abstract / framework description] Abstract and framework description: the claim that population evolution is governed primarily by the mass dependence of the accretion rate requires that accretion timescales are shorter than those of dynamical interactions and mergers, yet no quantitative comparison of these timescales is supplied for the gas-rich environments considered.
  2. [Abstract] Abstract: conclusions are stated to follow from analytical calculations and Monte Carlo population models, but the manuscript supplies neither explicit derivations of the continuity-equation solutions nor error analysis or direct comparison against observed catalogs, preventing verification that the math supports the stated claims.
minor comments (1)
  1. The exponent eta is introduced as a free parameter that controls the evolutionary outcome; a clearer mapping from specific physical accretion regimes (e.g., Bondi, Eddington-limited) to the adopted values of eta would strengthen the physical motivation.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for these constructive comments, which identify areas where the manuscript can be strengthened for clarity and verifiability. We respond to each major comment below and will revise the manuscript accordingly.

read point-by-point responses

  1. Referee: [Abstract / framework description] Abstract and framework description: the claim that population evolution is governed primarily by the mass dependence of the accretion rate requires that accretion timescales are shorter than those of dynamical interactions and mergers, yet no quantitative comparison of these timescales is supplied for the gas-rich environments considered.

    Authors: We agree that a quantitative timescale comparison is necessary to support the assumption that accretion dominates the evolution. In the revised manuscript we will add a new subsection (in the framework section) with order-of-magnitude estimates for accretion timescales in representative gas-rich environments (AGN disks, nuclear star clusters) and direct comparisons to literature values for dynamical friction, binary hardening, and merger timescales. This will delineate the parameter regime in which the continuity-equation description applies. revision: yes

  2. Referee: [Abstract] Abstract: conclusions are stated to follow from analytical calculations and Monte Carlo population models, but the manuscript supplies neither explicit derivations of the continuity-equation solutions nor error analysis or direct comparison against observed catalogs, preventing verification that the math supports the stated claims.

    Authors: The current text describes the continuity-equation approach and Monte Carlo results but does not provide step-by-step derivations or catalog comparisons. We will add an appendix containing the explicit analytical solutions to the continuity equation under power-law accretion, include sensitivity/error analysis for the Monte Carlo runs (e.g., variation with initial mass function and accretion duration), and insert a figure/table comparing the predicted high-mass tail and mass-ratio distribution to events in GWTC-3, with particular reference to GW231123. revision: yes

Circularity Check

0 steps flagged

No circularity: continuity-equation outcomes follow directly from assumed accretion law without reduction to fits or self-citations

full rationale

The paper applies a standard continuity-equation transport model in mass space to accretion with power-law dependence ˙m ∝ m^β. Different β values produce divergent or convergent evolution by direct integration of the continuity equation; these are explored via analytics and Monte Carlo sampling. No quoted step shows a parameter fitted to the target distribution and then relabeled as a prediction, nor any load-bearing self-citation or ansatz smuggled from prior work. The framework is self-contained against external benchmarks once the growth law and dominance assumption are stated; outcomes are model consequences rather than tautological redefinitions.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The central claim rests on treating accretion as the dominant transport process via a continuity equation whose behavior is set by the free parameter β; no new particles or forces are introduced.

free parameters (1)
  • β (accretion rate exponent)
    The mass dependence ˙m ∝ m^β is explored for values above and below 1 to determine whether evolution is divergent or convergent; its value is chosen according to the physical regime under consideration.
axioms (1)
  • domain assumption Compact-object population evolution obeys a continuity equation in mass space driven primarily by the accretion rate's mass dependence
    The framework is introduced in the abstract as the governing description, with other processes assumed secondary in gas-rich environments.

pith-pipeline@v0.9.1-grok · 5761 in / 1441 out tokens · 58452 ms · 2026-06-29T02:36:08.927766+00:00 · methodology

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