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arxiv: 2606.20393 · v1 · pith:C5RFU3EMnew · submitted 2026-06-18 · ✦ hep-ph · astro-ph.CO· astro-ph.HE

New Gauge Forces, Neutron Stars and Schwinger Neutrino Production

Yuxin Liu , Zhen Liu , Andrey Shkerin , Jing Shu , Yue Zhao This is my paper

Pith reviewed 2026-06-26 16:32 UTC · model grok-4.3

classification ✦ hep-ph astro-ph.COastro-ph.HE
keywords Lμ-Lτ gauge forceSchwinger pair productionneutron starsneutrino fluxlong-range forceselement abundancesB-L symmetryastrophysical constraints
0
0 comments X

The pith

For the Lμ-Lτ force with g ≳ 10^{-18}, Schwinger neutrino production in neutron stars alters their composition, suppresses charge, and invalidates merger constraints while producing a potentially detectable flux.

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

The paper investigates neutrino effects from new long-range forces obtained by gauging B-L, Le-Lμ/τ or Lμ-Lτ symmetries. Astronomical bodies generate leptonic potentials that trigger Schwinger pair production of the corresponding neutrinos. For the Lμ-Lτ case the effects become significant inside neutron stars once the gauge coupling reaches 10^{-18} or higher. The produced particles modify the star's element abundances and reduce its net Lμ-Lτ charge, removing the validity of merger-derived bounds at couplings above 10^{-17}. The escaping neutrinos carry typical energies of 100 MeV and could be observed from a young neutron star at roughly 100 pc, so a dedicated search would restore the tighter limit g ≲ 10^{-18}.

Core claim

For the Lμ-Lτ force these effects are significant in neutron stars if the gauge coupling is g≳10^{-18}. The muonic force changes the element abundances of a neutron star in equilibrium and suppresses its Lμ-Lτ charge. This invalidates the constraint on g from neutron star mergers, at g≳10^{-17}. Furthermore, for such values of g, the neutrino flux produced by the Schwinger effect could potentially be detected from a single young neutron star at a distance of ≃100 pc, with the typical neutrino energy Eν∼100 MeV. A dedicated search for such a signal will reassert the bound g≲10^{-18}.

What carries the argument

Schwinger pair production of neutrinos charged under the new gauge symmetry inside the leptonic potential well of a neutron star.

If this is right

  • The muonic force changes the element abundances of a neutron star in equilibrium.
  • It suppresses its Lμ-Lτ charge.
  • This invalidates the constraint on g from neutron star mergers at g≳10^{-17}.
  • The neutrino flux produced by the Schwinger effect could potentially be detected from a single young neutron star at a distance of ≃100 pc with typical energy Eν∼100 MeV.
  • A dedicated search for such a signal will reassert the bound g≲10^{-18}.

Where Pith is reading between the lines

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

  • Detection of the flux would open a new observational channel for ultra-weak gauge forces that bypasses laboratory limits.
  • The altered composition could modify other neutron-star observables such as cooling curves or maximum masses in ways left uncalculated here.
  • The same potential-driven production mechanism might operate in other dense objects once their internal potentials exceed the pair-creation threshold.

Load-bearing premise

Neutron-star equilibrium under the new force is reached solely through Schwinger pair production and element-abundance adjustment, without competing processes dominating the net Lμ-Lτ charge or composition.

What would settle it

Non-observation of the predicted 100 MeV neutrino flux from any young neutron star within about 100 pc, or direct evidence that neutron-star merger constraints remain valid at g > 10^{-17}, would show the Schwinger-driven suppression does not occur.

Figures

Figures reproduced from arXiv: 2606.20393 by Andrey Shkerin, Jing Shu, Yue Zhao, Yuxin Liu, Zhen Liu.

Figure 1
Figure 1. Figure 1: FIG. 1. The Mass-Radius relation in the presence of [PITH_FULL_IMAGE:figures/full_fig_p006_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. Distribution of muons [PITH_FULL_IMAGE:figures/full_fig_p007_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. The total [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4. Schematic plot showing the evolution of various chem [PITH_FULL_IMAGE:figures/full_fig_p008_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: ; see Appendix B 2. 8 This bound assumes that the universe was reheated to tempera￾tures above the muon mass. B. Bound on g from a nearby supernova neutrino afterglow Having just opened the window of the gauge couplings unconstrained by the NS binary mergers, we will now dis￾cuss how it can be prospectively closed again from non￾observation of the neutrino flux emitted by nearby NSs undergoing the process … view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6. Differential neutrino flux generated by the Schwinger [PITH_FULL_IMAGE:figures/full_fig_p010_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: FIG. 7. The GR correction to the 0’th component of the [PITH_FULL_IMAGE:figures/full_fig_p012_7.png] view at source ↗
read the original abstract

We investigate neutrino effects of new long-range forces arising from gauging $B-L$, $L_e-L_{\mu/\tau}$ or $L_{\mu}-L_{\tau}$ symmetries of the Standard Model. The leptonic potential generated by astronomical bodies, such as the Earth, the Sun or a neutron star, results in the Schwinger pair production of neutrinos charged under the new gauge symmetry. The oppositely charged particles accumulate in the potential well forming a degenerate Fermi gas, while equally charged particles fly away forming a steady flux of neutrinos. We find that, for the $B-L$ and $L_e-L_{\mu/\tau}$ forces, these effects are too weak to be observable. For the $L_{\mu}-L_{\tau}$ force these effects are significant in neutron stars if the gauge coupling is $g\gtrsim 10^{-18}$. The muonic force changes the element abundances of a neutron star in equilibrium and suppresses its $L_{\mu}-L_{\tau}$ charge. This invalidates the constraint on $g$ from neutron star mergers, at $g\gtrsim 10^{-17}$. Furthermore, for such values of $g$, the neutrino flux produced by the Schwinger effect could potentially be detected from a single young neutron star at a distance of $\simeq 100$ pc, with the typical neutrino energy $E_\nu\sim 100$ MeV. A dedicated search for such a signal will reassert the bound $g\lesssim 10^{-18}$.

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 examines neutrino production via the Schwinger effect induced by long-range potentials from new gauge forces associated with B-L, Le-Lμ/τ, and Lμ-Lτ symmetries. For B-L and Le-Lμ/τ the effects are stated to be unobservably weak. For Lμ-Lτ the manuscript claims that in neutron stars, gauge couplings g≳10^{-18} alter equilibrium element abundances, suppress the net Lμ-Lτ charge (thereby invalidating existing neutron-star-merger bounds at g≳10^{-17}), and generate a neutrino flux potentially detectable from a young neutron star at ~100 pc with typical energy ~100 MeV, allowing a dedicated search to restore the bound g≲10^{-18}.

Significance. If the central modeling assumptions are validated, the work would tighten phenomenological constraints on light Lμ-Lτ gauge bosons and identify a possible new astrophysical neutrino signal. The explicit linkage between charge suppression and invalidation of prior bounds, together with a concrete flux prediction, constitutes a falsifiable claim that could be tested with existing or near-future neutrino telescopes.

major comments (2)
  1. [neutron-star equilibrium section] The central claim that Schwinger pair production plus abundance adjustment suppresses the net Lμ-Lτ charge (thereby invalidating merger constraints for g≳10^{-17}) rests on the untested assertion that these channels dominate charge redistribution. No quantitative comparison of the Schwinger rate or abundance-adjustment timescale against competing processes (weak interactions in the core, magnetic-field effects, or accretion) is provided; without such a comparison the suppression and the consequent invalidation of prior bounds do not follow. (See the neutron-star equilibrium discussion and the paragraph containing the g≳10^{-17} statement.)
  2. [abstract and conclusions] The numerical thresholds quoted in the abstract (g≳10^{-18}, 100 pc, Eν∼100 MeV) and repeated in the conclusions are presented without an accompanying error budget, parameter scan, or explicit derivation from the Schwinger-rate formula. It is therefore impossible to determine whether these values are robust predictions or sensitive to the modeling choices for the neutron-star density profile and potential depth. (Abstract and final summary paragraph.)
minor comments (2)
  1. [throughout] Notation for the new gauge coupling is introduced as g but occasionally appears without a subscript; a consistent symbol (e.g., g_{Lμ-Lτ}) would improve readability.
  2. [introductory comparison paragraph] The statement that the effects are “too weak to be observable” for B-L and Le-Lμ/τ would benefit from a brief order-of-magnitude estimate or reference to the corresponding rate formula to allow the reader to reproduce the conclusion.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading of our manuscript and for providing constructive comments that will help improve the clarity and robustness of our results. We address each of the major comments below.

read point-by-point responses

  1. Referee: [neutron-star equilibrium section] The central claim that Schwinger pair production plus abundance adjustment suppresses the net Lμ-Lτ charge (thereby invalidating merger constraints for g≳10^{-17}) rests on the untested assertion that these channels dominate charge redistribution. No quantitative comparison of the Schwinger rate or abundance-adjustment timescale against competing processes (weak interactions in the core, magnetic-field effects, or accretion) is provided; without such a comparison the suppression and the consequent invalidation of prior bounds do not follow. (See the neutron-star equilibrium discussion and the paragraph containing the g≳10^{-17} statement.)

    Authors: We agree that a quantitative comparison between the Schwinger pair production rate, the abundance adjustment timescale, and competing processes is necessary to firmly establish that the Schwinger mechanism dominates the charge redistribution in neutron stars. The original manuscript emphasizes the novel effect but does not include explicit timescale comparisons. In the revised version, we will add estimates showing that for g ≳ 10^{-18}, the Schwinger-induced processes operate on timescales much shorter than those of weak interactions or accretion in the relevant regions, thereby justifying the suppression of the net Lμ-Lτ charge and the invalidation of the merger bounds at g ≳ 10^{-17}. revision: yes

  2. Referee: [abstract and conclusions] The numerical thresholds quoted in the abstract (g≳10^{-18}, 100 pc, Eν∼100 MeV) and repeated in the conclusions are presented without an accompanying error budget, parameter scan, or explicit derivation from the Schwinger-rate formula. It is therefore impossible to determine whether these values are robust predictions or sensitive to the modeling choices for the neutron-star density profile and potential depth. (Abstract and final summary paragraph.)

    Authors: The quoted values are order-of-magnitude estimates obtained by applying the Schwinger pair production rate to standard neutron star models with typical central densities and potential depths. While the manuscript derives them from the rate formula, we acknowledge the lack of a detailed error analysis or sensitivity study. In the revision, we will include a short discussion of the dependence on the density profile and provide a basic error budget to demonstrate the robustness of the thresholds g ≳ 10^{-18}, distance ∼100 pc, and Eν ∼100 MeV. revision: partial

Circularity Check

0 steps flagged

No significant circularity in derivation chain

full rationale

The paper calculates Schwinger pair production rates under new gauge forces in neutron stars, determines thresholds for observable effects on composition and neutrino flux, and discusses implications for existing merger constraints. These steps rely on physical modeling of potentials, pair production, and accumulation rather than reducing to self-definitional inputs, fitted parameters renamed as predictions, or load-bearing self-citations. The suppression of Lμ-Lτ charge and the proposed reassertion of bounds follow from the model's rate equations applied to neutron-star conditions; no equations or sections exhibit the specific reductions required for circularity flags. The derivation remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 1 invented entities

The central claim rests on the existence of unbroken gauged leptonic symmetries generating long-range potentials, the validity of the Schwinger mechanism in the stellar environment, and the assumption that equilibrium abundances adjust solely via the new force; no independent evidence for the new gauge boson is supplied.

free parameters (1)
  • gauge coupling g
    The thresholds g ≳ 10^{-18} and g ≳ 10^{-17} are the central parameters that set the onset of observable effects; their values are derived from the rate calculation rather than taken from external data.
axioms (2)
  • domain assumption The new U(1) symmetries remain exact and unbroken at stellar densities, producing truly long-range forces.
    Required for the potential to extend over neutron-star scales and trigger Schwinger production.
  • ad hoc to paper Schwinger pair production dominates over all other neutrino production and charge-redistribution channels inside the star.
    Implicit in the statement that the force 'suppresses its Lμ-Lτ charge' via abundance changes.
invented entities (1)
  • new gauge boson mediating Lμ-Lτ force no independent evidence
    purpose: Mediates the long-range leptonic force responsible for the stellar potential.
    Postulated new vector boson whose coupling g is the only free parameter controlling the effect.

pith-pipeline@v0.9.1-grok · 5818 in / 1794 out tokens · 45001 ms · 2026-06-26T16:32:18.979016+00:00 · methodology

discussion (0)

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Reference graph

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