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arxiv: 2410.12638 · v5 · submitted 2024-10-16 · 🌌 astro-ph.HE

Neutrino and pair creation in reconnection-powered coronae of accreting black holes

D. Karavola , M. Petropoulou , D. F. G. Fiorillo , L. Comisso , L. Sironi This is my paper

Pith reviewed 2026-05-23 19:07 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords neutrinospair productionAGN coronablack hole accretionmagnetic reconnectionhadronic processesIceCube observations
0
0 comments X

The pith

Relativistic protons in accreting black hole coronae produce enough pairs for observed optical depths above a critical accretion rate.

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

The paper models how relativistic protons accelerated in current sheets around black holes affect the pair content and neutrino production in AGN coronae. It identifies two key parameters: proton magnetization σ_p setting neutrino energies, and the X-ray Eddington ratio λ_X,Edd controlling energy transfer to secondaries. Above a critical λ_X,Edd, proton-photon interactions and gamma-gamma annihilation create sufficient electron-positron pairs to match the Thomson optical depths of 0.1-10 seen in coronae. Below the threshold, hadronic processes fall short, and neutrino luminosity follows a quadratic scaling with X-ray luminosity rather than linear.

Core claim

Relativistic protons accelerated in black-hole magnetospheric current sheets drive pair enrichment and neutrino emission in AGN coronae through proton-photon interactions and γγ annihilation. For λ_X,Edd above a critical value that depends on σ_p, these processes yield enough secondary pairs to reach τ_T of 0.1-10. The neutrino luminosity scales as L_X squared over L_Edd below the critical rate and linearly with L_X above it. The model is applied to Seyfert galaxies including NGC 1068 in the context of IceCube data.

What carries the argument

The combination of proton magnetization σ_p, which sets the neutrino peak energy, and the X-ray Eddington ratio λ_X,Edd, which governs energy transfer to secondary particles via hadronic and electromagnetic cascades.

If this is right

  • For λ_X,Edd ≳ λ_Edd,crit, hadronic interactions suffice to produce the coronal pairs.
  • Neutrino luminosity scales quadratically with L_X at low Eddington ratios and linearly at high ratios.
  • The model applies to observed Seyfert galaxies to predict neutrino fluxes consistent with or testable by IceCube.
  • Below the critical rate, coronal pairs must come from other mechanisms besides proton interactions.

Where Pith is reading between the lines

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

  • This suggests that neutrino detections could help measure the magnetization in black hole coronae.
  • The scaling relations could be tested with multi-messenger observations of AGN populations.
  • If extended to other accretion states, it might explain why some sources are neutrino-bright while others are not.

Load-bearing premise

That relativistic protons are accelerated in the black hole magnetospheric current sheets with a magnetization value that directly controls both the neutrino spectrum peak and the fraction of energy going into secondary pairs.

What would settle it

Detection of a high neutrino flux from an AGN with λ_X,Edd below the predicted critical value, or a measurement of coronal optical depth inconsistent with the pair production rate at high λ_X,Edd.

read the original abstract

A ubiquitous feature of accreting black hole systems is their hard X-ray emission which is thought to be produced through Comptonization of soft photons by electrons and positrons in the vicinity of the black hole, in a region with optical depth of order unity. The origin and composition of this Comptonizing region, known as the corona, is a matter open for debate. In this paper we investigate the role of relativistic protons accelerated in black-hole magnetospheric current sheets for the pair enrichment and neutrino emission of AGN coronae. Our model has two free parameters, namely the proton plasma magnetization $\sigma_{\rm p}$, which controls the peak energy of the neutrino spectrum, and the Eddington ratio $\lambda_{\rm X, Edd}$ (defined as the ratio between X-ray luminosity $L_{\rm X}$ and Eddington luminosity $L_{\rm Edd}$), which controls the amount of energy transferred to secondary particles. For sources with $\lambda_{\rm X, Edd} \gtrsim \lambda_{\rm Edd, crit}$ (where $\lambda_{\rm Edd, crit} \sim 10^{-1}$ for $\sigma_{\rm p}=10^5$ or $\sim 10^{-2}$ for $\sigma_{\rm p}=10^7$), proton-photon interactions and $ \gamma \gamma$ annihilation produce enough secondary pairs to achieve Thomson optical depths $\tau_{\rm T} \sim 0.1-10$. In the opposite case of $\lambda_{\rm X, Edd} \lesssim \lambda_{\rm Edd, crit}$, the coronal pairs cannot originate only from hadronic interactions. Additionally, we find that the neutrino luminosity scales as $L^2_{\rm X}/L_{\rm Edd}$ for $\lambda_{\rm X, Edd} \lesssim \lambda_{\rm Edd, crit}$, while it is proportional to $L_{\rm X}$ for higher $\lambda_{\rm X, Edd}$ values. We apply our model to four Seyfert galaxies, including NGC 1068, and discuss our results in light of recent IceCube 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 presents a two-parameter model (proton magnetization σ_p and X-ray Eddington ratio λ_X,Edd) for pair enrichment and neutrino emission in black-hole coronae powered by reconnection-accelerated protons. It reports that above a critical Eddington ratio λ_Edd,crit(σ_p) (∼10^{-1} for σ_p=10^5 or ∼10^{-2} for σ_p=10^7), pγ interactions and γγ annihilation yield secondary pairs sufficient for Thomson optical depths τ_T∼0.1–10; below this threshold pairs cannot originate solely from hadronic processes. Neutrino luminosity is found to scale as L_ν∝L_X²/L_Edd for λ_X,Edd≲λ_Edd,crit and L_ν∝L_X above it. The model is applied to four Seyfert galaxies including NGC 1068 and discussed against IceCube data.

Significance. If the scalings and thresholds hold under the stated assumptions, the work supplies a concrete mechanism connecting magnetospheric reconnection to both corona pair content and observable neutrino output, with explicit luminosity scalings that could be tested against multi-messenger data. The explicit mapping from reconnection physics (via σ_p) to neutrino peak energy and secondary production is a positive feature, though the two free parameters limit the strength of any external predictions.

major comments (2)
  1. [Abstract / model setup] Abstract and model-setup paragraph: the headline result that τ_T reaches 0.1–10 for λ_X,Edd≳λ_Edd,crit is load-bearing for the central claim, yet λ_Edd,crit is defined directly in terms of the two free parameters σ_p and λ_X,Edd. Consequently the threshold is a contour in parameter space rather than an independent prediction; applications to NGC 1068 and other Seyferts therefore require external justification for the chosen σ_p values.
  2. [Abstract] Abstract: the reported neutrino-luminosity scalings (L_ν∝L_X²/L_Edd below λ_Edd,crit and L_ν∝L_X above) are stated as direct consequences of the same two parameters; the manuscript should clarify whether these scalings remain robust when σ_p is varied over the range explored or whether they are fixed by construction once σ_p and λ_X,Edd are chosen.
minor comments (1)
  1. [Abstract] Notation for λ_Edd,crit should be introduced with an explicit functional dependence on σ_p already in the abstract to avoid the impression of an externally derived critical value.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive comments. We address each major point below and indicate where revisions will be made to improve clarity.

read point-by-point responses

  1. Referee: [Abstract / model setup] Abstract and model-setup paragraph: the headline result that τ_T reaches 0.1–10 for λ_X,Edd≳λ_Edd,crit is load-bearing for the central claim, yet λ_Edd,crit is defined directly in terms of the two free parameters σ_p and λ_X,Edd. Consequently the threshold is a contour in parameter space rather than an independent prediction; applications to NGC 1068 and other Seyferts therefore require external justification for the chosen σ_p values.

    Authors: We agree that λ_Edd,crit is a contour in the (σ_p, λ_X,Edd) parameter space, as the model is explicitly constructed with these two free parameters. The headline result demonstrates the conditions under which hadronic processes can supply the observed τ_T; it is not presented as an independent prediction. For the applications to NGC 1068 and other Seyferts, the chosen σ_p values (10^5–10^7) are representative of the high-magnetization regime expected from magnetospheric reconnection. We will revise the abstract and model-setup section to emphasize the parametric nature of the threshold and add a brief physical motivation for the σ_p range based on reconnection physics. revision: partial

  2. Referee: [Abstract] Abstract: the reported neutrino-luminosity scalings (L_ν∝L_X²/L_Edd below λ_Edd,crit and L_ν∝L_X above) are stated as direct consequences of the same two parameters; the manuscript should clarify whether these scalings remain robust when σ_p is varied over the range explored or whether they are fixed by construction once σ_p and λ_X,Edd are chosen.

    Authors: The scalings arise from the energy partitioning and interaction rates (pγ and pair production) in the model and are not fixed by construction. We have verified that the L_ν ∝ L_X²/L_Edd (below threshold) and L_ν ∝ L_X (above threshold) forms hold across the full explored range of σ_p. We will add a clarifying sentence in the abstract or results section noting this robustness with respect to σ_p variations. revision: yes

Circularity Check

0 steps flagged

No significant circularity; results explicitly parametric in stated free parameters.

full rationale

The paper explicitly states it has two free parameters (σ_p controlling neutrino peak energy, λ_X,Edd controlling energy transfer to secondaries) and derives λ_Edd,crit(σ_p) and the L_ν scalings as functions of these inputs and the resulting optical depth regimes. This is standard parametric modeling with conditional outcomes; no quoted reduction of a claimed prediction to a fitted input by construction, no self-definitional loop (e.g., X defined via Y), and no load-bearing self-citation chain. The derivation remains self-contained against the model's own equations and assumptions without external benchmarks being required for the internal consistency check.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central claim rests on two free parameters that directly set all reported thresholds and scalings, plus the domain assumption that protons are accelerated in magnetospheric current sheets.

free parameters (2)
  • proton plasma magnetization σ_p
    Controls the peak energy of the neutrino spectrum; two example values (10^5, 10^7) are used to set λ_Edd,crit.
  • Eddington ratio λ_X,Edd
    Controls the amount of energy transferred to secondary particles; determines whether the source is above or below the critical threshold.
axioms (2)
  • domain assumption Relativistic protons are accelerated in black-hole magnetospheric current sheets
    Stated as the physical basis enabling proton-photon interactions in the corona.
  • standard math Proton-photon interactions and γγ annihilation produce secondary electron-positron pairs
    Standard particle-physics processes invoked without derivation in the abstract.

pith-pipeline@v0.9.0 · 5940 in / 1533 out tokens · 40946 ms · 2026-05-23T19:07:40.017628+00:00 · methodology

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Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. Single-source-class interpretation of the diffuse astrophysical neutrino flux

    astro-ph.HE 2026-03 unverdicted novelty 4.0

    The diffuse astrophysical neutrino flux is interpreted as dominated by a single source class with dominant pγ production for target photon temperatures of 0.1-1 keV.

Reference graph

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