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arxiv: 2606.29830 · v1 · pith:2UNFB2BGnew · submitted 2026-06-29 · 🌌 astro-ph.HE

Constraints on Hadronic Emission from Microquasars Detected by LHAASO

V. Vecchiotti , E. Amato , G. Giacinti , G. Morlino , G. Peron This is my paper

Pith reviewed 2026-06-30 05:37 UTC · model grok-4.3

classification 🌌 astro-ph.HE
keywords microquasarsLHAASOultra-high-energy gamma rayshadronic emissioncosmic-ray contributionPeVatronsdiffusion propagationGalactic cosmic rays
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The pith

Hadronic interactions cannot explain the full ultra-high-energy gamma-ray emission detected by LHAASO from any of the six microquasars.

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

The authors test whether cosmic rays accelerated in microquasars produce the observed gamma rays through collisions with ambient gas. They adopt a diffusion-dominated transport model in which the diffusion coefficient is reduced near each source and equals the standard Galactic value farther out, with continuous particle injection lasting 0.1 to 1 million years. For every source that shows emission above 100 TeV the predicted hadronic gamma-ray flux lies below the LHAASO measurements unless the acceleration efficiency is raised above 10 percent in two cases. The same models limit the combined contribution of the detected sources to roughly 4 percent of the Galactic cosmic-ray intensity at 1 PeV under standard assumptions, rising to 37 percent only when efficiency is set to the highest value still allowed by the gamma-ray data. Sources without ultra-high-energy detections add at most 17 percent even under the most generous injection timescale.

Core claim

Microquasars detected by LHAASO at ultra-high energies cannot have their gamma-ray emission fully explained by hadronic interactions alone. Using a diffusion-dominated propagation model with suppressed diffusion near the source and continuous injection over 0.1-1 Myr, the calculated hadronic gamma-ray flux is insufficient to match observations for any source. The contribution of these sources to the Galactic cosmic-ray spectrum at 1 PeV is limited to approximately 4% for standard parameters, or up to 37% when using the maximum acceleration efficiency permitted by the gamma-ray data.

What carries the argument

Diffusion-dominated cosmic-ray propagation with a spatially varying diffusion coefficient (suppressed near the source) together with measured gas densities and continuous injection over 0.1-1 Myr, used to compute expected hadronic gamma-ray yields and the resulting contribution to the PeV cosmic-ray spectrum.

If this is right

  • Hadronic emission alone is insufficient to account for the observed ultra-high-energy gamma rays in all six detected sources.
  • The detected microquasars contribute at most 4 percent to the Galactic cosmic-ray spectrum at 1 PeV under 10 percent efficiency and 0.1 Myr injection.
  • Raising acceleration efficiency to the gamma-ray upper limit raises the contribution to 37 percent.
  • Injection lasting 1 Myr would exceed existing cosmic-ray observational bounds.
  • Non-detected sources are limited to a maximum 17 percent contribution under the longest injection time considered.

Where Pith is reading between the lines

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

  • If leptonic processes dominate the gamma-ray output, coordinated radio and X-ray monitoring could reveal synchrotron or inverse-Compton components that distinguish them from hadronic emission.
  • The required suppression of diffusion near the sources points to local magnetic structures whose effect could be tested with targeted particle-transport simulations.
  • Applying the same modeling framework to other candidate Galactic PeVatrons would tighten the overall budget of cosmic rays at the knee.

Load-bearing premise

Cosmic rays spread outward mainly by diffusion whose coefficient is lower close to the microquasar than the average Galactic value, and the surrounding gas densities are taken from published maps.

What would settle it

A measurement showing that the actual gas density within a few parsecs of any detected microquasar is high enough, or that the local diffusion coefficient is low enough, for hadronic emission at 10 percent efficiency to reproduce the full LHAASO flux would falsify the conclusion that hadronic processes fall short.

Figures

Figures reproduced from arXiv: 2606.29830 by E. Amato, G. Giacinti, G. Morlino, G. Peron, V. Vecchiotti.

Figure 1
Figure 1. Figure 1: Comparison of diffusion and advection timescales over a region of 50 pc. The red solid (dashed) line shows the diffu￾sion timescale for the Galactic (suppressed) diffusion coefficient. The black solid, dashed, and dotted lines represent the advection timescales for an advection velocity of v = 0.08 c (comparable to the jet velocity) and for wind velocity v = 300 km s−1 and v = 3000 km s−1 , respectively. e… view at source ↗
Figure 2
Figure 2. Figure 2: Estimated target density required to reproduce the [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Contribution to the CR proton spectrum for the microquasars detected by LHAASO in the di [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Same as Figure [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Same as Fig.2 but for the microquasars undetected by LHAASO. The predictions for GRO J0422+32, XTE J1118+480 and Cygnus X-1 overlap. 5. Discussion We find that, under standard assumptions for the CR acceler￾ation efficiency, the UHE gamma-rays measured by LHAASO can only be partially explained by p − p interactions. The small hadronic contribution inferred for V4641 Sgr is consistent with the conclusions o… view at source ↗
Figure 6
Figure 6. Figure 6: Upper limit on the contribution to the CR spectrum for the microquasars undetected for LHAASO. The left (right) panel [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗
read the original abstract

Recently, the LHAASO collaboration reported ultra-high-energy (UHE) gamma rays from six microquasars. For five of these sources, the emission extends beyond $100$ TeV, making microquasars promising candidates for Galactic PeVatrons. We investigate whether gamma-rays around $100$ TeV originate from hadronic interactions of accelerated cosmic rays (CRs) with the ambient medium, and we estimate the contribution of these sources to the measured CR spectrum around the knee. We also place upper limits on six LHAASO microquasars with no detected UHE emission. We assume diffusion-dominated propagation of CR, with a diffusion coefficient suppressed compared to the average Galactic value near the source and equal to the Galactic value at large distances. We assume continuous injection over timescales of $t_{\rm age}=0.1-1$ Myrs. Using available measurements of the gas density, we find that hadronic interactions alone cannot fully account for the observed emission for any of the detected sources. However, in the case of GRS 1915+105 and MAXI J1820+070, the hadronic scenario may still be valid when considering acceleration efficiency higher than $10\%$. We then derive upper limits on the hadronic contribution to the observed gamma-ray flux. We estimate that the detected sources contribute at most $\sim4\%$ of the Galactic CR spectrum at $1$ PeV for an injection timescales of $0.1$ Myrs and a CR acceleration efficiency of $10 \%$. When adopting the maximum acceleration efficiency allowed by the gamma-ray observations the contribution rises to $37\%$. Longer injection timescales ($\sim 1$ Myrs) lead to contributions exceeding the observational constraints. For sources not detected at UHE, we obtained a maximum contribution of $\sim 17\%$, achieved assuming continuous injection over $1$ Myr.

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 paper claims that hadronic interactions of cosmic rays from six LHAASO-detected microquasars cannot fully account for the observed UHE gamma-ray emission when using published gas-density measurements and a diffusion-dominated propagation model (diffusion coefficient suppressed near the source, Galactic value at large distances, continuous injection over 0.1–1 Myr). For GRS 1915+105 and MAXI J1820+070 the hadronic scenario remains possible at efficiencies >10%. The detected sources contribute at most ~4% to the Galactic CR spectrum at 1 PeV (0.1 Myr, 10% efficiency), rising to 37% at the maximum efficiency allowed by the gamma-ray data; longer injection times exceed constraints. Upper limits are also derived for six non-detected sources (max ~17% at 1 Myr).

Significance. If the modeling assumptions hold, the work supplies quantitative upper limits on the hadronic contribution of microquasars to the PeV CR knee, indicating they are sub-dominant and favoring leptonic channels for the LHAASO fluxes. Credit is due for anchoring the calculation to independent published gas-density data rather than fitting to the gamma-ray fluxes themselves and for producing explicit percentage contributions under stated parameter choices.

major comments (2)
  1. [§3] §3 (propagation and interaction modeling): the central claim that hadronic emission 'cannot fully account' for any detected source rests on the adopted n_gas values without reported uncertainties or alternative maps; because the gamma-ray yield scales linearly with n_gas, an underestimate by a factor of ~2 would allow 10% efficiency to match the fluxes, directly affecting the 'cannot fully account' statement.
  2. [Results section] Results section on CR spectrum contribution: the quoted 4% and 37% figures are presented without propagated uncertainties on the diffusion suppression factor or explicit sensitivity tests to the position-dependent D(r); the abstract itself notes the absence of error bars and explicit D values, which is load-bearing for the quantitative upper-limit claim.
minor comments (2)
  1. [Abstract] Abstract: include at least the range of diffusion coefficients and the specific gas-density references used so that the numerical claims can be assessed without the full methods section.
  2. Notation: the injection timescale is written both as t_age and t_inj in different paragraphs; standardize to a single symbol.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their thoughtful comments and for acknowledging the significance of our work in providing quantitative upper limits on the hadronic contribution of microquasars to the PeV cosmic-ray spectrum. We address each major comment below.

read point-by-point responses

  1. Referee: [§3] §3 (propagation and interaction modeling): the central claim that hadronic emission 'cannot fully account' for any detected source rests on the adopted n_gas values without reported uncertainties or alternative maps; because the gamma-ray yield scales linearly with n_gas, an underestimate by a factor of ~2 would allow 10% efficiency to match the fluxes, directly affecting the 'cannot fully account' statement.

    Authors: We agree that the adopted gas density values are central to our conclusions and that their uncertainties should be addressed. The densities are taken from published measurements as cited in the manuscript. We will revise §3 to include the reported uncertainties from those references where available and add a sensitivity analysis showing the impact of varying n_gas by factors of 2 on the required efficiencies and the 'cannot fully account' statement. This will make the dependence explicit without altering the baseline results. revision: yes

  2. Referee: [Results section] Results section on CR spectrum contribution: the quoted 4% and 37% figures are presented without propagated uncertainties on the diffusion suppression factor or explicit sensitivity tests to the position-dependent D(r); the abstract itself notes the absence of error bars and explicit D values, which is load-bearing for the quantitative upper-limit claim.

    Authors: We acknowledge that the quantitative upper limits would be strengthened by explicit sensitivity tests. The diffusion model parameters are fixed as described in §3 (suppressed D near the source transitioning to Galactic value). We will add a new subsection or appendix with sensitivity tests varying the suppression factor (e.g., by factors of 2-10) and the transition radius, reporting the resulting range in CR contribution percentages. This addresses the lack of propagated uncertainties while maintaining the baseline values under our stated assumptions. revision: yes

Circularity Check

0 steps flagged

No significant circularity; derivation uses independent external inputs

full rationale

The paper's central results rest on comparing hadronic gamma-ray yields (linear in independently measured n_gas) against LHAASO fluxes, then scaling the implied CR injection to the Galactic spectrum. Gas densities are taken from published measurements, not fitted or defined from the gamma-ray data under analysis. Diffusion suppression and injection timescales are stated modeling assumptions, not derived from the target observables. No self-citation chain, self-definitional loop, or renaming of a fitted quantity as a prediction appears in the provided text. The derivation chain therefore remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

3 free parameters · 3 axioms · 0 invented entities

The central claim rests on three standard astrophysical assumptions plus three adjustable parameters whose specific numerical values are not supplied in the abstract. No new physical entities are introduced.

free parameters (3)
  • diffusion-coefficient suppression factor near source
    Chosen to represent local conditions; numerical value not stated.
  • injection timescale t_age
    Scanned over 0.1–1 Myr; treated as a free parameter.
  • CR acceleration efficiency
    Baseline 10%; upper values allowed by gamma-ray data also considered.
axioms (3)
  • domain assumption Cosmic-ray transport is diffusion-dominated
    Invoked to model propagation from the microquasar.
  • domain assumption Injection is continuous over the source lifetime
    Used to integrate the cosmic-ray population.
  • domain assumption Published gas-density measurements are accurate and representative
    Required to compute interaction rates.

pith-pipeline@v0.9.1-grok · 5901 in / 1599 out tokens · 46122 ms · 2026-06-30T05:37:27.450131+00:00 · methodology

discussion (0)

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