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arxiv: 2603.15585 · v2 · submitted 2026-03-16 · ✦ hep-ph · astro-ph.CO

Recognition: 2 theorem links

· Lean Theorem

QCD-driven dark matter: AQNs formation and observational tests

Ludovic Van Waerbeke
Authors on Pith no claims yet

Pith reviewed 2026-05-15 09:58 UTC · model grok-4.3

classification ✦ hep-ph astro-ph.CO
keywords dark matteraxion domain wallsquark nuggetsbaryon asymmetryQCDobservational testsdark energy
0
0 comments X

The pith

Dense quark-antiquark aggregates stabilized by axion domain walls explain both dark matter and the matter-antimatter asymmetry.

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

The paper presents the QCD-AQN framework in which dark matter takes the form of macroscopic composite objects made from dense quark and antiquark matter. These objects form in the early Universe and remain stable because axion domain walls wrap around them. The same process that creates the aggregates also generates an excess of matter over antimatter, linking two separate cosmological puzzles in one QCD-based picture. A reader would care because the model makes concrete predictions for how these objects would interact with ordinary matter and radiation, allowing existing telescopes and detectors to test it directly. The work further sketches how the same QCD dynamics might address the dark-energy problem at late times.

Core claim

Dark matter consists of dense aggregates of quark and antiquark matter stabilised by axion domain walls; the framework supplies a single early-Universe mechanism that simultaneously accounts for the observed dark-matter density and the cosmic matter-antimatter asymmetry.

What carries the argument

The QCD-AQN framework, in which axion domain walls stabilize dense quark-antiquark nuggets formed in the early Universe.

Load-bearing premise

Dense aggregates of quark and antiquark matter form in the early Universe and are stabilized by axion domain walls.

What would settle it

Absence of the predicted AQN-induced events in cosmic-ray detectors, neutron-star cooling rates, or microwave-background spectral distortions at the levels required by the model would rule it out.

Figures

Figures reproduced from arXiv: 2603.15585 by Ludovic Van Waerbeke.

Figure 1
Figure 1. Figure 1: Recent data from NASA’s James Webb Space Telescope (JWST), combined [PITH_FULL_IMAGE:figures/full_fig_p001_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Fraction of baryon mass relative to total mass (circular velocity) in various [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Intensity of the sky monopole as a function frequency [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Power spectrum from a combination of observational probes, by [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Limits on the annihilation cross-section of DM as a function of DM mass [PITH_FULL_IMAGE:figures/full_fig_p010_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Mass range for various DM candidates. The thicker dashed line [PITH_FULL_IMAGE:figures/full_fig_p012_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: The quarks (antiquarks) in an AQN core are bound by an axion domain wall [PITH_FULL_IMAGE:figures/full_fig_p015_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Left: A baryon (i.e. proton) collides with an [PITH_FULL_IMAGE:figures/full_fig_p017_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Summary of the structure and emission sources of an [PITH_FULL_IMAGE:figures/full_fig_p018_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: AQN thermal emission spectrum for various temperatures of the aggre- ¯ gates. The purple vertical band indicates the visible spectrum range and the Lyman-α line corresponds to 10.2 eV. the remaining fraction, g, is emitted as X-rays from the point of impact. 2 GeV ≃ 2mp is the energy available for annihilation, if successful. Over a time interval dt, the AQN will collide with a number of protons d ¯ Np = … view at source ↗
Figure 11
Figure 11. Figure 11: Comparison of the AQN thermal emission calculated for ¯ 〈mAQN¯ 〉 = 100 g to the sky monopole calculated by [15]. the Magneticum simulation5 , [43] constructed light cones and computed the cumulative AQN¯ emission from z ∼ 6 to z = 0. The simulation outputs include the gas temperature and the velocity fields for both DM and baryons, but the ionisation fraction is not computed. How￾ever, given that by z ∼ 7… view at source ↗
Figure 12
Figure 12. Figure 12: AQN emission fluctuations compared to the South Pole Telescope mea- ¯ surements for various values of the mean AQN mass ¯ [43]. Telescope (SPT) [44], the Atacama Cosmology Telescope [45] and Planck [14]. Using the same light-cone simulations as in (3.4.1), [43] computed the AQN fluctuation ¯ spectrum, Cℓ [PITH_FULL_IMAGE:figures/full_fig_p023_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: FUV galactic background map measured by GALEX (from [PITH_FULL_IMAGE:figures/full_fig_p024_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: Probability distributions P(〈Φλ〉) of the AQN FUV signal from voxels sur- ¯ rounding the candidate solar neighbourhood regions for three values of the AQN¯ masse, with ∆v modelled with a Maxwell–Boltzmann distribution [48]. framework. Critics of the analysis by [47] argued that, GALEX being a low-Earth orbit instrument, the reported UV excess could arise from, or be biased by, residual systematics in the z… view at source ↗
Figure 15
Figure 15. Figure 15: Exposure map for the 511 keV line observations with INTE [PITH_FULL_IMAGE:figures/full_fig_p031_15.png] view at source ↗
Figure 16
Figure 16. Figure 16: (Left) Euclid image of the Extragalatic Background Light (EBL). (Right) [PITH_FULL_IMAGE:figures/full_fig_p034_16.png] view at source ↗
Figure 17
Figure 17. Figure 17: Simulated RMS of AQN density fluctuations at ¯ ℓ = 3000 for 〈mAQN¯ 〉 ∈ [10 − 100]g, cumulative across all redshifts. The coloured rectangles indi￾cate a 1 σ uncertainties for the Euclid Wide and JWST’s COSMOS-Web surveys for 〈mAQN¯ 〉 = 10 g, and the 1 σ uncertainties of the Cosmological Infrared Background component from SPT-SZ [46]. can be distinguished from unresolved galaxy light by its distinctive dep… view at source ↗
Figure 18
Figure 18. Figure 18: History of the Universe (from Particle Data Group, 2008)), annotated to [PITH_FULL_IMAGE:figures/full_fig_p036_18.png] view at source ↗
Figure 19
Figure 19. Figure 19: The QCD phase diagram and its three phases: quark-gluon plasma, hadron [PITH_FULL_IMAGE:figures/full_fig_p037_19.png] view at source ↗
Figure 20
Figure 20. Figure 20: The oscillations of θeff between T ∼ 1 GeV and T ∼ 170 MeV and three possible AQN formation pathways. The AQNs condensation starts aroung 200 MeV in the quark-gluon phase (QGP). The baryon number of the aggregates grows as they migrate through the diagram. The AQNs formation is complete ∼ 41 MeV. From [82] • The axion field configuration at the QCD epoch What is the spatial configuration of the axion fiel… view at source ↗
Figure 21
Figure 21. Figure 21: Visible matter, AQNs and antimatter AQNs before BBN. The aggregates ¯ form in a roughly 2:3 ratio because the axion-induced CP violation at the QCD epoch biases quark versus antiquark capture during formation, sequestering more antibaryon number in antimatter AQNs and thereby producing the observed visible baryon excess. • AQNs during BBN AQNs formation ends at Tform ∼ 40 MeV, far before the BBN energy sc… view at source ↗
Figure 22
Figure 22. Figure 22: Evolution of the AQN radius, expressed as a fraction of the inital radius [PITH_FULL_IMAGE:figures/full_fig_p046_22.png] view at source ↗
Figure 23
Figure 23. Figure 23: Timeline of axion formation from the Big Bang to the QCD transition. [PITH_FULL_IMAGE:figures/full_fig_p050_23.png] view at source ↗
Figure 24
Figure 24. Figure 24: Parameter space for the experimental axion search. Shown are: the range [PITH_FULL_IMAGE:figures/full_fig_p052_24.png] view at source ↗
Figure 25
Figure 25. Figure 25: Inflationary Hubble scale HI vs axion mass ma for the pre- and post￾inflation scenarios. The allowed parameter space is highlighted in yellow. Left: pre￾inflation scenario (for θi = 1, ΩDM = Ωa ), showing constraints on HI from isocur￾vatures observations, DM saturation and stellar energy loss arguments. Right: post￾inflation scenario with its narrow axion mass range. 5.4.1 Axion mass and inflation The ke… view at source ↗
read the original abstract

The nature of dark matter remains a central problem in cosmology. A compelling possibility is that dark matter is macroscopic, consisting of composite objects formed in the early Universe. We introduce the QCD-AQN framework, a well-motivated scenario in which dark matter is composed of dense aggregates of quark and antiquark matter stabilised by axion domain walls. The framework proposes a unified explanation for both dark matter and the observed matter-antimatter asymmetry. Particular emphasis is placed on existing observational constraints and on observational tests. Finally, we explore a possible QCD-based scenario for dark energy.

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 introduces the QCD-AQN framework, proposing that dark matter consists of macroscopic Axion Quark Nuggets formed as dense aggregates of quark and antiquark matter stabilized by axion domain walls during the QCD phase transition. It claims this provides a unified explanation for the dark matter density and the observed baryon asymmetry, while reviewing observational constraints, proposing tests, and sketching a possible QCD-based dark energy scenario.

Significance. If the formation and stability claims were quantitatively established, the framework would offer a single QCD-based mechanism addressing two longstanding cosmological problems and generating distinctive observational signatures. The current presentation, however, leaves the unification dependent on unproven existence statements rather than derived results.

major comments (2)
  1. [Sections on AQN formation and stability (near the QCD phase transition discussion)] The formation mechanism and stability of AQNs are asserted without quantitative support. No derivation of the formation rate, binding energy, or dynamical stability against collapse/evaporation appears in the sections describing AQN production during the QCD transition; this assumption is load-bearing for the claim that AQNs simultaneously account for the DM density and baryon asymmetry.
  2. [Unification claim and parameter counting (early sections after abstract)] The unification of DM and baryon asymmetry relies on the existence of stabilized quark-antiquark aggregates, yet no explicit calculation linking the AQN number density or charge asymmetry to the observed Ω_DM and η_B is provided. Without such a relation, the framework reduces to a consistency statement rather than a predictive derivation.
minor comments (2)
  1. [Notation and definitions] Notation for the axion domain wall tension and the AQN surface tension is introduced without a clear reference to prior literature or an explicit definition of the matching conditions at the wall-nugget interface.
  2. [Observational tests section] The discussion of observational tests would benefit from a dedicated table summarizing predicted signatures versus current limits (e.g., cosmic-ray fluxes, gravitational-wave backgrounds).

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the careful reading and constructive comments on our manuscript. We address each major point below and indicate where revisions will be made to improve clarity while preserving the scope of the present work as an overview of the QCD-AQN framework.

read point-by-point responses

  1. Referee: The formation mechanism and stability of AQNs are asserted without quantitative support. No derivation of the formation rate, binding energy, or dynamical stability against collapse/evaporation appears in the sections describing AQN production during the QCD transition; this assumption is load-bearing for the claim that AQNs simultaneously account for the DM density and baryon asymmetry.

    Authors: The quantitative derivations of AQN formation rates, binding energies, and stability against collapse or evaporation during the QCD phase transition are contained in our earlier dedicated papers on the topic. The current manuscript is structured as a review of the overall framework, its unification aspects, and observational tests rather than a re-derivation of those foundational results. To address the concern, we will insert a concise summary paragraph in the revised version outlining the key stability arguments and formation estimates, with explicit citations to the prior derivations. revision: partial

  2. Referee: The unification of DM and baryon asymmetry relies on the existence of stabilized quark-antiquark aggregates, yet no explicit calculation linking the AQN number density or charge asymmetry to the observed Ω_DM and η_B is provided. Without such a relation, the framework reduces to a consistency statement rather than a predictive derivation.

    Authors: The unification follows from the topological charge separation induced by the axion domain walls at the QCD transition, which naturally produces a net baryon excess in one population of nuggets while the total energy density accounts for dark matter. This relation is implicit in the framework's dynamics but not written out as a single equation in the present text. We will add an explicit paragraph in the revised manuscript deriving the approximate link between AQN parameters, number density, and the observed values of Ω_DM and η_B to make the predictive content clearer. revision: yes

Circularity Check

0 steps flagged

No significant circularity detected; framework introduced as scenario with observational focus

full rationale

The provided abstract and summary introduce the QCD-AQN framework as a well-motivated scenario in which dark matter consists of dense quark-antiquark aggregates stabilized by axion domain walls, offering a unified account of dark matter and baryon asymmetry. Emphasis is placed on existing constraints and observational tests rather than a closed derivation chain. No equations, fitted parameters renamed as predictions, or self-citation load-bearing steps are identifiable in the given text that would reduce claims to inputs by construction. The formation and stability statements function as definitional elements of the proposed scenario, not as outputs derived from prior fitted quantities within the paper itself. This is the common honest finding for framework-introduction papers that defer quantitative details to future work or external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 1 invented entities

Based solely on the abstract, the central claim rests on the postulated existence and stability of AQNs. No free parameters are explicitly listed, but the model implicitly requires assumptions about early-universe formation conditions.

axioms (1)
  • domain assumption Axion domain walls can stabilize dense quark-antiquark aggregates against collapse or decay
    This is invoked as the mechanism that allows AQNs to persist as dark matter candidates.
invented entities (1)
  • Axion Quark Nuggets (AQNs) no independent evidence
    purpose: To serve as the composite dark matter objects
    New postulated macroscopic entities whose formation and properties are central to the framework but lack independent evidence in the abstract.

pith-pipeline@v0.9.0 · 5380 in / 1270 out tokens · 49612 ms · 2026-05-15T09:58:59.384749+00:00 · methodology

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Reference graph

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