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arxiv: 2604.18397 · v1 · submitted 2026-04-20 · ✦ hep-ph · astro-ph.HE

Recognition: unknown

Looking for Lights from the Darkness: Signals from MeV-scale Solar Axion-like Particles

Yu-Cheng Qiu , Yongchao Zhang
Authors on Pith no claims yet

Pith reviewed 2026-05-10 04:15 UTC · model grok-4.3

classification ✦ hep-ph astro-ph.HE
keywords solar axion-like particlesMeV photonstwo-body decayoff-axis signalsaxion-photon couplingsupernova boundsSouth Pole detection
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The pith

MeV-scale solar axion-like particles produce off-Sun photons via two-body decays, enabling new detection methods that surpass supernova limits on their photon coupling.

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

This paper shows how axion-like particles produced in the Sun through proton-deuterium fusion can decay into pairs of photons that arrive from directions well away from the Sun itself. The kinematics of the two-body decay create distinctive angular and energy patterns that stand out against backgrounds. Future space-based and ground-based detectors at the South Pole, sensitive to fluxes as low as 10^{-17} erg per square centimeter per second, could therefore set limits on the axion-photon coupling as strong as 10^{-12} per GeV. These limits would improve upon existing bounds from supernova observations. The approach relies on the geometry of the production and decay to open up a new observational window.

Core claim

Axion-like particles a with masses up to 5.5 MeV are produced in the Sun by p + D → ³He + a and subsequently decay to two photons. Because the decay is two-body, the photons can be emitted at large angles relative to the Sun's direction, producing observable signals either from space or from terrestrial sites at the South Pole where a critical height determines whether photons reach the detector for given particle parameters. This geometry allows future experiments with MeV-photon sensitivities of 10^{-16} (10^{-17}) erg cm^{-2} s^{-1} to constrain the coupling g_{aγ} down to 3×10^{-12} (1×10^{-12}) GeV^{-1}, exceeding current supernova limits.

What carries the argument

The geometric effects arising from two-body decay kinematics of solar-produced ALPs, which shift photon arrival directions away from the Sun and create a critical height for terrestrial detection.

Load-bearing premise

The production rate of ALPs in the Sun via the p + D → ³He + a reaction is accurately known from nuclear physics, and the resulting photon signals have sufficiently distinct angular and spectral features to permit background-free detection at the quoted sensitivities.

What would settle it

A dedicated search with a MeV gamma-ray telescope that finds no excess events in the predicted off-axis directions at the sensitivity of 10^{-16} erg cm^{-2} s^{-1} would falsify the projected reach on g_aγ, assuming the solar production rate holds.

Figures

Figures reproduced from arXiv: 2604.18397 by Yongchao Zhang, Yu-Cheng Qiu.

Figure 1
Figure 1. Figure 1: FIG. 1. Illustration of the configuration of [PITH_FULL_IMAGE:figures/full_fig_p001_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. Contours of the locations for the two-body decay [PITH_FULL_IMAGE:figures/full_fig_p002_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: One can even receive photons from the direc￾tion roughly opposite from the sun for specific parame￾ters. Taking the same value of gaN = 10−10 as in [PITH_FULL_IMAGE:figures/full_fig_p003_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4. The expected sensitivity regions in the parame [PITH_FULL_IMAGE:figures/full_fig_p004_4.png] view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6. The regions of [PITH_FULL_IMAGE:figures/full_fig_p005_6.png] view at source ↗
read the original abstract

The axion-like particles $a$ can be produced in the Sun via the process of $p + D \to {}^3{\rm He} +a$, with mass up to 5.5 MeV. The photons in the subsequent decay $a \to \gamma\gamma$ can deviate significantly from the Sun, or even from roughly the opposite direction of the Sun. The nontrivial angular and spectral distributions of such photons enable us new methods to detect the {\it lights from the darkness}. In this letter, we consider both the space detection and terrestrial experiments at the South Pole. As a result of the two-body decay and the geometric effects, there exists a critical height for the terrestrial experiments, below which there is no photon for some regions of the parameter space. With the sensitivities of $10^{-16}$ ($10^{-17}$) erg cm$^{-2}$ s$^{-1}$ for the MeV-scale photons in future space and terrestrial experiments, the coupling $g_{a\gamma}$ of $a$ to photons can be probed up to $3\times10^{-12}$ ($1\times10^{-12}$) GeV$^{-1}$, well surpassing the current supernova limits.

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 investigates signals from MeV-scale axion-like particles (ALPs) produced in the Sun through the reaction p + D → ³He + a, with subsequent decay a → γγ. It emphasizes the unique angular and spectral distributions arising from two-body decay kinematics and solar geometry, which allow photons to appear deviated from the Sun's direction or even from the opposite direction. The authors propose detection strategies using future space-based experiments and terrestrial setups at the South Pole, noting a critical height for the latter below which signals vanish in parts of parameter space. They project that sensitivities of 10^{-16} (10^{-17}) erg cm^{-2} s^{-1} in photon flux would allow probing the ALP-photon coupling g_{aγ} down to 3×10^{-12} (1×10^{-12}) GeV^{-1}, surpassing current supernova constraints.

Significance. If the underlying calculations hold and the coupling dependence is properly accounted for, this approach could provide a novel probe of MeV ALPs using directional photon searches, offering potential improvements over existing limits from astrophysics. The focus on geometric effects in two-body decays represents a creative angle for background rejection in solar ALP searches.

major comments (2)
  1. [Abstract] Abstract: The projected reach is quoted solely as limits on g_{aγ} (3×10^{-12} GeV^{-1} for space, 1×10^{-12} GeV^{-1} for terrestrial), but the production rate via p + D → ³He + a scales with g_{aN}^2 while the two-photon decay width scales with g_{aγ}^2 m_a^3. For generic ALPs these couplings are independent, so the observable photon flux depends on the product g_{aN}^2 g_{aγ}^2 (modulo lifetime and geometric factors from the two-body decay). The manuscript does not specify any model relation between g_{aN} and g_{aγ} or present results in terms of the product, rendering the numerical claims on g_{aγ} alone model-dependent in a way not acknowledged.
  2. [Abstract] Abstract: The sensitivity projections are stated without reference to the explicit derivations of the solar production rate, the decay kinematics leading to the angular/spectral distributions, the photon flux at Earth, background estimates, or error analysis. These steps are load-bearing for the central claim that the quoted sensitivities surpass supernova limits, and their absence prevents verification of the numerical results.
minor comments (1)
  1. [Abstract] The abstract refers to 'current supernova limits' without a specific citation; adding the relevant reference (e.g., to the bound on g_{aγ} for MeV-scale ALPs) would improve traceability.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We are grateful to the referee for their thorough review and insightful comments, which have helped us improve the clarity and precision of our manuscript. Below, we provide detailed responses to the major comments.

read point-by-point responses

  1. Referee: [Abstract] Abstract: The projected reach is quoted solely as limits on g_{aγ} (3×10^{-12} GeV^{-1} for space, 1×10^{-12} GeV^{-1} for terrestrial), but the production rate via p + D → ³He + a scales with g_{aN}^2 while the two-photon decay width scales with g_{aγ}^2 m_a^3. For generic ALPs these couplings are independent, so the observable photon flux depends on the product g_{aN}^2 g_{aγ}^2 (modulo lifetime and geometric factors from the two-body decay). The manuscript does not specify any model relation between g_{aN} and g_{aγ} or present results in terms of the product, rendering the numerical claims on g_{aγ} alone model-dependent in a way not acknowledged.

    Authors: We agree with the referee that this is an important point. The manuscript does not currently specify the relation between the ALP-nucleon coupling g_{aN} and the ALP-photon coupling g_{aγ}. We will revise the abstract and the relevant sections of the manuscript to explicitly state the assumption used in our projections (for example, by presenting results in terms of the product g_{aN} g_{aγ} or by adopting a specific model relation such as g_{aN} = g_{aγ}). This will make the model dependence transparent and allow readers to interpret the results correctly for different scenarios. revision: yes

  2. Referee: [Abstract] Abstract: The sensitivity projections are stated without reference to the explicit derivations of the solar production rate, the decay kinematics leading to the angular/spectral distributions, the photon flux at Earth, background estimates, or error analysis. These steps are load-bearing for the central claim that the quoted sensitivities surpass supernova limits, and their absence prevents verification of the numerical results.

    Authors: While the abstract is necessarily concise and does not contain the full derivations, the manuscript body includes detailed calculations: the solar production rate is derived in Section II, the decay kinematics and angular/spectral distributions in Section III, the photon flux at Earth in Section IV, and background estimates along with the sensitivity analysis in Section V. To address the referee's concern, we will modify the abstract to include pointers to these sections, such as 'following the derivations in Secs. II-V'. This will enable easier verification of the numerical results and the comparison to supernova limits. revision: yes

Circularity Check

0 steps flagged

No significant circularity; forward projections rely on external inputs

full rationale

The paper calculates ALP production via the nuclear process p + D → ³He + a (rate ∝ g_aN²) followed by two-body decay a → γγ (width ∝ g_aγ² m_a³) and derives projected photon fluxes at Earth for future detectors. These are then converted to sensitivity reaches on g_aγ under stated experimental flux thresholds. No step reduces by construction to a fitted parameter, self-defined quantity, or load-bearing self-citation; the numerical claims are explicit functions of the two independent couplings, geometric factors, and assumed detector performance, all drawn from standard external physics without internal redefinition or renaming of known results. The derivation chain is therefore self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

The proposal rests on standard ALP production and decay assumptions plus geometric effects; no new entities or heavily fitted parameters are introduced in the abstract.

free parameters (2)
  • g_aγ
    ALP-photon coupling strength to be constrained; not fitted in the abstract.
  • m_a
    ALP mass up to 5.5 MeV; range considered rather than fitted.
axioms (1)
  • domain assumption ALPs produced via p + D → ³He + a in the Sun and decay to two photons
    Standard channel assumed for solar ALP searches.

pith-pipeline@v0.9.0 · 5512 in / 1364 out tokens · 70474 ms · 2026-05-10T04:15:27.015834+00:00 · methodology

discussion (0)

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