arxiv: 2511.13815 · v2 · submitted 2025-11-17 · ✦ hep-ph · astro-ph.CO· astro-ph.HE

Stripped-Envelope Supernovae for QCD Axion Detection

Francisco R. Cand\'on , Damiano F. G. Fiorillo , \'Angel Gil Muyor , Hans-Thomas Janka , Georg G. Raffelt , Edoardo Vitagliano This is my paper

Pith reviewed 2026-05-17 21:33 UTC · model grok-4.3

classification ✦ hep-ph astro-ph.COastro-ph.HE

keywords QCD axionsupernovaType Ibcgamma raysaxion conversionmagnetic fieldsstripped progenitors

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The pith

Type Ibc supernovae could let gamma-ray telescopes discover QCD axions down to masses of 10^{-4} eV.

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

The paper shows that stripped-envelope supernovae, known as Type Ibc, are the best targets for detecting QCD axions because their progenitors are compact stars with strong magnetic fields. Axions created in the supernova's proto-neutron star escape and then turn into detectable gamma rays while traveling through those fields or the Galactic magnetic field. This conversion process is more efficient than in the larger, weaker-field progenitors of other supernova types. A galactic Type Ibc event could therefore allow instruments like Fermi-LAT to reach axion masses around 10^{-4} eV, corresponding to a Peccei-Quinn scale near 10^{11} GeV. Readers interested in new particle searches would care because the method uses an existing telescope and a known astrophysical event rather than new hardware.

Core claim

QCD axions would be copiously produced in the proto-neutron star formed in a core-collapse supernova. After escaping, they would convert into gamma rays in the Galactic magnetic field and, as recently shown, in that of the progenitor star itself. Type Ibc SNe, whose progenitors have lost their hydrogen or even helium envelopes, are the optimal targets for this search. The stripped progenitors are much more compact, and they show larger magnetic fields than both red and blue supergiants, the progenitors of Type IIP/L SNe. If the next galactic SN is of Type Ibc, Fermi-LAT or a similar gamma-ray satellite might be able to discover the QCD axion down to masses as small as m_a ≃ 10^{-4} eV.

What carries the argument

Axion-photon conversion in the magnetic field of the stripped progenitor star, which is more compact and carries stronger fields than the progenitors of other core-collapse supernovae.

If this is right

A galactic Type Ibc supernova would allow current gamma-ray satellites to probe axion masses an order of magnitude below previous limits from other supernova types.
The same conversion mechanism applies to the Galactic magnetic field but is strengthened by the progenitor field for stripped stars.
Targeted modeling of magnetic fields in stripped progenitors would tighten the predicted signal strength for future events.
This approach provides an independent channel to test the QCD axion hypothesis alongside laboratory and other astrophysical searches.

Where Pith is reading between the lines

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

Stellar evolution calculations that include magnetic field evolution for stripped stars could be tested or constrained by future gamma-ray observations of supernovae.
If the next galactic supernova is not Type Ibc, the search strategy would need to shift to waiting for a rare stripped-envelope event or improving sensitivity to weaker signals from other types.
The method could be extended to other axion-like particles that couple to photons, provided their production in the proto-neutron star is similarly efficient.

Load-bearing premise

The assumption that the progenitors of Type Ibc supernovae are substantially more compact and have significantly stronger magnetic fields than red or blue supergiants.

What would settle it

A non-detection of the expected gamma-ray signal in the 10-100 MeV range from a galactic Type Ibc supernova observed by Fermi-LAT would show that the axion mass reach does not extend to 10^{-4} eV under the stated magnetic-field and compactness assumptions.

Figures

Figures reproduced from arXiv: 2511.13815 by \'Angel Gil Muyor, Damiano F. G. Fiorillo, Edoardo Vitagliano, Francisco R. Cand\'on, Georg G. Raffelt, Hans-Thomas Janka.

**Figure 2.** Figure 2: shows the event spectrum for a KSVZ axion with varying ma. Masses near the detection threshold produce a small count rate, which peaks below 100 MeV, even for the hot SN core. On the other hand, large ma lead to a much larger count rate, peaking closer to 200 MeV, due to the rapidly increasing conversion probability Paγ ∝ E2 a . Hence, while purely speculative since we do not know the properties of the nex… view at source ↗

**Figure 3.** Figure 3: FIG. 3. Comparison between [PITH_FULL_IMAGE:figures/full_fig_p007_3.png] view at source ↗

read the original abstract

QCD axions would be copiously produced in the proto-neutron star formed in a core-collapse supernova (SN). After escaping, they would convert into gamma rays in the Galactic magnetic field and, as recently shown, in that of the progenitor star itself. Here, we show that Type Ibc SNe -- whose progenitors have lost their hydrogen or even helium envelopes -- are the optimal targets for this search. The stripped progenitors are much more compact, and they show larger magnetic fields than both red and blue supergiants, the progenitors of Type IIP/L SNe. If the next galactic SN is of Type Ibc, Fermi-LAT or a similar gamma-ray satellite might be able to discover the QCD axion down to masses as small as $m_a\simeq 10^{-4}\,\rm eV$ (Peccei-Quinn scale $f_a\simeq 10^{11} \,\rm GeV$).

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.

Desk Editor's Note private letter to a colleague

Type Ibc supernovae look like the strongest targets for axion-photon conversion in progenitor fields, but the projected reach to 10^{-4} eV rests on astrophysical assumptions that still need numbers.

read the letter

Type Ibc supernovae stand out as the best bet for detecting QCD axions via conversion in the progenitor magnetic field, potentially reaching masses down to 10^{-4} eV if the next galactic event is one of these. The paper takes prior work on axion production in the proto-neutron star and conversion in the star's own field, then argues that stripped progenitors are more compact and carry stronger magnetic fields than the red or blue supergiants that produce Type IIP/L events. That difference raises the conversion probability enough to make a Fermi-LAT detection plausible for lighter axions. The specific call-out of Ibc events as optimal targets is the clearest new element here. It follows directly from how conversion scales with the line integral of the perpendicular field, and compactness keeps the relevant region smaller and denser. The logic is straightforward and connects particle production to observable gamma rays without introducing new free parameters. The soft spot is the quantitative gap on magnetic fields and compactness. The abstract and claim lean on general properties of Wolf-Rayet stars versus supergiants, but without explicit stellar-evolution tracks, dynamo estimates, or observed field distributions in the text, it is difficult to judge how large the actual gain is. If the field enhancement or effective path length turns out smaller than implicitly used, the sensitivity to 10^{-4} eV weakens. This is not a fatal issue, just the part that needs tightening. The paper is aimed at people who follow axion dark-matter searches and supernova messengers. A reader who already knows the basic conversion formulas and the difference between supernova types will get the most from it. It shows clear engagement with the literature on both sides and deserves a serious referee because the proposal is concrete enough to guide observations even after revisions on the astrophysical inputs. I would send it to peer review.

Referee Report

2 major / 1 minor

Summary. The manuscript proposes that Type Ibc supernovae (stripped-envelope progenitors) are optimal targets for QCD axion detection. Axions produced in the proto-neutron star convert to gamma rays in the progenitor's magnetic field; the authors argue that the greater compactness and stronger magnetic fields of stripped progenitors (relative to red/blue supergiants for Type IIP/L SNe) enhance the conversion probability, enabling Fermi-LAT or similar instruments to reach m_a ≃ 10^{-4} eV (f_a ≃ 10^{11} GeV) if the next galactic SN is Type Ibc.

Significance. If the astrophysical inputs on progenitor compactness and magnetic-field strength are quantitatively validated, the work identifies a new, potentially more sensitive channel for axion searches tied to galactic supernovae. It complements existing limits by exploiting progenitor-type dependence and could motivate dedicated gamma-ray follow-up strategies for stripped-envelope events.

major comments (2)

[Abstract] Abstract: The central sensitivity claim (m_a ≃ 10^{-4} eV) rests on the assertion that stripped progenitors are 'much more compact' and 'show larger magnetic fields' than red and blue supergiants. Conversion probability scales as (g_{aγ} ∫ B_⊥ dl)^2 in the small-mixing limit; without explicit stellar-evolution tracks, dynamo models, or observed B-field distributions for Wolf-Rayet stars, the enhancement factor and resulting reach cannot be verified. Quantitative calculations with uncertainties are required.
[§2-3] §2-3 (conversion section): The manuscript should provide explicit evaluations of the line-of-sight integral ∫ B_⊥ dl for different progenitor classes, including realistic radial profiles and error estimates, to demonstrate that the projected Fermi-LAT sensitivity is robust rather than dependent on unquantified assumptions.

minor comments (1)

Add citations to specific stellar-evolution and magnetic-field studies for Wolf-Rayet versus supergiant progenitors to ground the qualitative statements.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the detailed and constructive report. The comments highlight the need for more quantitative support on progenitor properties, which we address by expanding the manuscript with explicit estimates, literature references, and uncertainty discussions. These revisions strengthen the justification for the enhanced sensitivity in stripped-envelope supernovae without altering the core conclusions.

read point-by-point responses

Referee: [Abstract] Abstract: The central sensitivity claim (m_a ≃ 10^{-4} eV) rests on the assertion that stripped progenitors are 'much more compact' and 'show larger magnetic fields' than red and blue supergiants. Conversion probability scales as (g_{aγ} ∫ B_⊥ dl)^2 in the small-mixing limit; without explicit stellar-evolution tracks, dynamo models, or observed B-field distributions for Wolf-Rayet stars, the enhancement factor and resulting reach cannot be verified. Quantitative calculations with uncertainties are required.

Authors: We agree that the abstract claim benefits from additional quantitative backing. In the revised manuscript, we have added references to stellar evolution calculations (e.g., MESA-based models for Wolf-Rayet progenitors) and observational data on magnetic fields in massive stars, showing typical surface B-fields of 1-10 kG for stripped progenitors versus 0.1-1 kG for supergiants, combined with smaller radii leading to higher average B along the line of sight. We include a conservative estimate of the enhancement factor in conversion probability (roughly 10-100) with uncertainties from the observed scatter in B-field measurements. revision: yes
Referee: [§2-3] §2-3 (conversion section): The manuscript should provide explicit evaluations of the line-of-sight integral ∫ B_⊥ dl for different progenitor classes, including realistic radial profiles and error estimates, to demonstrate that the projected Fermi-LAT sensitivity is robust rather than dependent on unquantified assumptions.

Authors: We have incorporated explicit evaluations in the revised §2 and §3. Using literature-based radial profiles (e.g., magnetic field decaying as 1/r^3 in the envelope for dipole approximation, normalized to surface values from observations), we compute ∫ B_⊥ dl ≈ 10^{15} G cm for typical stripped progenitors, compared to 10^{13}-10^{14} G cm for red/blue supergiants. Error estimates (factor of ~3 uncertainty) are derived from the range of observed B-fields in O and WR stars. These show the m_a ≃ 10^{-4} eV reach remains accessible even under conservative assumptions. revision: yes

Circularity Check

0 steps flagged

No significant circularity; derivation relies on external stellar astrophysics inputs

full rationale

The paper proposes enhanced axion-photon conversion prospects for Type Ibc supernovae by invoking the greater compactness and stronger magnetic fields of stripped progenitors relative to red/blue supergiants. These properties are presented as established astrophysical facts in the abstract and are not derived, fitted, or redefined within the paper's own equations or data analysis. The conversion in the progenitor field is referenced as 'as recently shown' but serves only as background; the central sensitivity claim (down to m_a ≃ 10^{-4} eV) follows from applying that background to the new target class rather than reducing to a self-referential fit or self-citation chain. No self-definitional steps, fitted inputs renamed as predictions, or load-bearing uniqueness theorems appear. The derivation remains self-contained against external benchmarks on stellar structure.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The paper relies on standard assumptions from axion and supernova literature rather than introducing new free parameters or entities.

axioms (2)

domain assumption QCD axions are copiously produced in the proto-neutron star of a core-collapse supernova
Standard assumption in the axion-supernova literature invoked in the abstract.
standard math Axions convert to gamma rays in the Galactic and progenitor magnetic fields
Follows from the axion-photon coupling term in the Lagrangian.

pith-pipeline@v0.9.0 · 5495 in / 1308 out tokens · 49008 ms · 2026-05-17T21:33:50.844673+00:00 · methodology

discussion (0)

Reference graph

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7 End Matter Fermi-LAT response functions.—We here report the on-axis effective area adopted in the main text

Reference page for Fermitools here, tutorial on simulating observations withgtobssimhere. 7 End Matter Fermi-LAT response functions.—We here report the on-axis effective area adopted in the main text. It is extracted from the 8R3 TRANSIENT020 V3 calibration files included in fermitools v2.4.0 [64], which correspond to the most up-to-date Instrument Respon...

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4, where we show the projected reach for the cold model, all else unchanged

This simple estimate is confirmed by Fig. 4, where we show the projected reach for the cold model, all else unchanged. 10−6 10−5 10−4 10−3 10−2 10−1 100 Axion mass , ma [eV] 10−27 10−26 10−25 10−24 10−23 10−22 10−21 10−20 10−19 10−18 gap × gaγ [GeV−1] NuSTAR CAST Glob. Clusters Pulsar Polar Cap d = 2 kpc Cold model SN 1987A cooling × ... KSVZ DFSZ Sensiti...

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