Gamma Rays from SN1987A due to Pseudoscalar Conversion

E. Masso; J. A. Grifols; R. Toldra

REVIEW

Gamma Rays from SN1987A due to Pseudoscalar Conversion

J. A. Grifols, E. Masso, R. Toldra

Astrophysics · Submitted 5 Jun 1996 · 18 references

Pith's verdict: A real factor-of-three improvement on the ultralight pseudoscalar-photon coupling, but the quoted 3e-12 is a model-dependent estimate rather than a precision bound.

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arXiv IDastro-ph/9606028 (version 1)

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CitationE. Masso, J. A. Grifols, R. Toldra. "Gamma Rays from SN1987A due to Pseudoscalar Conversion." arXiv:astro-ph/9606028 (1996). https://pith.science/paper/WAKNXZO4

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Editor's note

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Worth your time if you track axion-like-particle bounds. The new number is g < 3e-12 GeV^-1 for m < 1e-9 eV, from the SMM/GRS null observation of SN1987A, roughly a factor of three below Carlson and Krasnikov. The observational channel is the genuinely new part; the production and mixing machinery is standard and properly cited to Raffelt and to Raffelt-Stodolsky, and the paper says so rather than dressing it up. The chain is arithmetically consistent: I redid Phi times P times Delta t and got about 2e-12 before the spectral integral, which lands where the quoted 3e-12 does once Eq. 15 is included. The production calculation is done with more care than most: Primakoff on protons with explicit screening wavenumbers, and explicit arguments for why the electron and nucleon-nucleon channels are suppressed. The band integral in Eq. 15 also handles the fact that the spectrum runs past the 100 MeV GRS cutoff, so the truncation is accounted for rather than waved away. The authors are upfront about the mass range and about the spectral shape. Nothing here is circular; the bound rests on an external measurement plus published formalism, with no tuned parameters. The soft spot is the conversion probability. P goes as (B_T L)^2, so g goes as (B_T L)^-1/2, and B_T = 1 microgauss comes from projecting an assumed 2 microgauss toroidal model onto the SN1987A line of sight. Calling L = 1 kpc conservative against a stated coherence length of several kpc is fine in direction, but the paper never varies the field and never shows what a domain-structured field does to the sin(x)/x factor. The stated error budget, a factor of 2 from core density, propagates to g as only about 1.2 and does not touch the field at all. So read 3e-12 as a model-dependent estimate; the honest range is maybe 2 to 5e-12. That is still a real improvement, just not a precision number. A smaller point: the suppression arguments for e-gamma and pn -> pn gamma phi are qualitative, which is fine for a bound but would need checking before anyone tried to tighten it. This is for people tracking ALP astrophysical limits and for anyone planning a supernova gamma-ray search with GLAST or Fermi. Send it out; it is a legitimate short paper. I would ask the referees to request a field-variation scan and an explicit statement of how the bound moves with B_T and L.

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Major objections (2)

[Pseudoscalar conversion, Eqs. (19)–(25)] The conversion probability P = (1/4) g² B_T² L² (sin x/x)² with B_T = 1 μG and L = 1 kpc is the single input that sets the quoted bound, since g scales as (B_T L)^{-1/2}. The paper calls L = 1 kpc 'conservative' relative to a coherence length of 'several kiloparsecs' [16], but it never shows the domain-averaged result. For a field made of N domains of length L_c with random orientations the amplitudes add in quadrature and P ≈ (1/4) g² B² L_c L_total, which for L_total of a few kpc and L_c = 1 kpc exceeds the single-domain estimate, so the choice is in fact conservative; but this should be stated explicitly. As written, a reader cannot tell whether the quoted 3×10^{-12} GeV^{-1} survives a factor-of-two change in the assumed field. I would ask the authors to add a short paragraph giving the domain-random-walk scaling and to quote the bound for, say, B_T = 0.5, 1, 2 μG and L_c = 0.3, 1, 3 kpc.
[Results and Conclusions, Eq. (27) and the sentence 'we estimate an uncertainty factor of 2 in the limit (27)'] The stated uncertainty budget covers only the variation of the core density and temperature, and it is not propagated correctly: a factor-of-two change in the core parameters enters the flux and hence moves g by only 2^{1/4} ≈ 1.2. The field model of Eqs. (24)–(25), the choice Δt = 5 s, and the truncation of the spectrum to the 25–100 MeV band are not propagated at all, even though the bound scales as (B_T L)^{-1/2} and as (Δt)^{-1/4}. A factor-of-two field uncertainty alone shifts the bound by about 1.4. The result should therefore be quoted as a range, for example g < (2–5)×10^{-12} GeV^{-1}, with the individual contributions to the budget separated, rather than as the single number in Eq. (27).

Minor objections (10)

[Pseudoscalar production, text preceding Eq. (14)] The proton density is printed as n_p = 1.4×10^{-38} cm^{-3}, which is inconsistent both with the 1.4×10^{38} cm^{-3} used in Eq. (14) and with the quoted p_F = 320 MeV; the exponent should be corrected.
[Eq. (15)] The numerical value of f(ξ², E_min, E_max) is never given. With ξ = κ/2T ≈ 0.42 and x running from 0.42 to 1.67 I estimate f ≈ 0.13, and this factor is what turns the crude estimate of about 2×10^{-12} GeV^{-1} into the quoted 3×10^{-12} GeV^{-1}. Please quote f explicitly so that Eq. (27) can be reproduced.
[Eq. (11)] The correlation term Z_i Z_j α T exp(−κr)/r is dimensionally inconsistent: α/r is already dimensionless, so the term should carry 1/T rather than T. Please check the expression.
[Eq. (13)] The quotient defining ε is written without parentheses and is ambiguous as typeset; please add them so that the numerator and denominator are unambiguous.
[Eq. (22)] The electron-density normalization is printed as 'n_e ≃ 0.03 cm 3' and should read cm^{-3}.
[Introduction, sentence on Krasnikov [10]] The coupling is printed as 'g ∼ 10^{-11} GeV^{-11}' and should read GeV^{-1}.
[Eq. (23)] The coherence condition is stated as m ≤ 10^{-9} eV, but the actual requirement is Δ_osc L ≪ 1, which for ω = 25 MeV and L = 1 kpc gives m ≪ 2×10^{-7} eV. The stated condition is therefore conservative, and the paper could note that the bound extends to larger masses and indicate where the sin(x)/x suppression begins to degrade it.
[Results and Conclusions, final paragraph] The claim that EGRET and GLAST 'could be able to detect' a signal for allowed g is not quantified. A short estimate of the expected photon count for g near the bound, using the stated effective areas and energy ranges, would make the observational prospect concrete.
[Eq. (6)] The notation σ(ω) v n_p dn_γ(T,ω) is loose, since n_p is a density rather than part of the photon distribution; please write the thermal average explicitly.
[Pseudoscalar production, free-streaming assumption] The paper should state that the φ mean free path in the core is much larger than R_c for the g values considered, so that the free-streaming assumption used to write Eq. (14) is justified.

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The paper

The paper claims

A light pseudoscalar particle produced in the core of SN1987A would partly turn into gamma rays in the galactic magnetic field, and the Solar Maximum Mission's failure to see any such signal caps the particle's coupling to two photons at $g

The reading

The paper asks a sharp question: if a very light pseudoscalar particle couples to two photons, a core-collapse supernova should be a bright source of it, and the galaxy's magnetic field should convert a small fraction of that stream back into gamma rays on the way to Earth. SN1987A is the test case, because the Gamma-Ray Spectrometer on the Solar Maximum Mission was watching when the neutrino burst arrived in 1987 and recorded no excess gamma-ray flux in the 25 to 100 MeV band. Turning that null result into a bound, the authors conclude $g < 3.5$ (in units of $10^{-12}$ GeV$^{-1}$), roughly a factor of three below the limits they cite from pulsar polarimetry, x-ray conversion in giant-star cores, and x-ray background isotropy. The claim matters because it covers the mass range $m < 10^{-9}$ eV, where laboratory and cosmological arguments are weak and where axion models do not force the coupling to be tiny. The authors also point out that EGRET, and later GLAST, would be sensitive to the whole emission spectrum and could actually see the converted signal for couplings the bound still allows.

What carries the argument

The load-bearing mechanism is photon-pseudoscalar oscillation in a transverse magnetic field, combined with Primakoff production in a degenerate plasma. The conversion probability is $P(phi to gamma) = (1/4) g^2 B_T^2 L^2 (sin x / x)^2$, with $x$ set by the plasmon mass and the particle mass; for $m < 10^{-9}$ eV the oscillation is coherent and the $sin x / x$ factor goes to one, so the whole bound becomes a clean product of production rate, mixing probability, and observing time. The production side uses a screened Primakoff cross section, where the plasma cuts off the Coulomb potential beyond a screening length set by proton Debye and electron Thomas-Fermi wave numbers. The elegance of the construction is that both the production and the conversion scale as $g^2$, so the null flux limit translates directly into a bound on $g$ rather than on some combination of parameters.

Extended reading notes

Core claim

The central claim is a new astrophysical upper bound on the pseudoscalar-photon coupling, $g < 3.5$ (in units of $10^{-12}$ GeV$^{-1}$), valid for particle masses below $10^{-9}$ eV. The argument has three multiplicative pieces. First, pseudoscalars are produced in the hot, dense proto-neutron star through the Primakoff process $p + gamma to p + phi$, with a flux at Earth of about $3.5$ (in units of $10^{4}$ cm$^{-2}$ s$^{-1}$) for $g = 10^{-11}$ GeV$^{-1}$, scaled by core radius, proton density, temperature, and distance. Second, a fraction of that flux converts to photons in the galactic field, with probability about $3.5$ (in units of $10^{-3}$) for the same coupling, a $1$ microgauss transverse field, and a $1$ kpc coherence length. Third, multiplying by a conservative 5 s emission window and requiring the product to stay under the SMM/GRS limit of $0.6$ cm$^{-2}$ gives the bound. The authors estimate a factor-of-two uncertainty from the unknown supernuclear equation of state, and note that the pseudoscalars drain at most $10^{-4}$ of the neutrino energy budget, so they do not back-react on the collapse.

Load-bearing premise

The conversion step assumes a single uniform transverse galactic field of about 1 microgauss coherent over 1 kpc along the line of sight to SN1987A, a modelled rather than measured field whose value enters the bound directly.

Editorial extensions

If this is right

Any pseudoscalar with mass below $10^{-9}$ eV and coupling above $3.5$ (in units of $10^{-12}$ GeV$^{-1}$) is excluded by the absence of a gamma-ray excess at SN1987A in the SMM data.
A nearby core collapse observed by EGRET, or later by GLAST, could detect the converted photon signal outright for couplings the bound still permits, since those instruments cover the full emission spectrum up to tens of GeV.
Because the conversion probability is mass-independent in this regime, the bound applies to any ultralight pseudoscalar coupled to two photons, not only to axions with a specific mass-coupling relation.
The expected photon spectrum peaks somewhat above $2.7 T$, around 160 MeV, so part of the signal fell outside the GRS 100 MeV cutoff and the quoted bound is conservative in that respect.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

The bound scales as $(B_T L)^{-1/2}$, so a better measurement of the galactic field along the SN1987A line of sight would move the number without any new gamma-ray data at all; the field model, not the detector, is the current bottleneck.
Because the signal is a prompt, few-second gamma-ray flash coincident with a neutrino burst, a positive detection would be a clean two-messenger signature, distinguishable from ordinary supernova gamma-ray emission by its hard spectrum and its lack of a shock-powered tail.
A galactic supernova at, say, 10 kpc instead of 55 kpc would raise the flux by roughly a factor of thirty, probing couplings an order of magnitude below the present limit with the same kind of instrument.
The same production-and-conversion logic could be applied to other dense photon sources with known distances, such as neutron-star cores or the early universe, though the magnetic-field uncertainties would have to be handled case by case.

Original abstract

A light pseudoscalar coupled to two photons would be copiously emitted by the core of a supernova. Part of this flux would be converted to $\gamma-$rays by the galactic magnetic field. Measurements on the SN1987A $\gamma-$ray flux by the Gamma-Ray Spectrometer on the Solar Maximum Mission satellite already imply a bound on the coupling $g < 3 \times 10^{-12}$ GeV$^{-1}$. The improved generation of satellite-borne detectors, like EGRET or the project GLAST, could be able to detect a pseudoscalar-to-photon signal from a nearby supernova, for allowed values of $g$.

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Compiled by classifier-1.13-20260917 via OpenRouter, question bank abstract-p1-20260923, 2026-09-23: 1 request, 3,676 input tokens, $0.0002 reported.

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arXiv listing abstract v1. Results and the main claim are underlined; show every role.

A light pseudoscalar coupled to two photons would be copiously emitted by the core of a supernova. Part of this flux would be converted to $\gamma-$rays by the galactic magnetic field. Measurements on the SN1987A $\gamma-$ray flux by the Gamma-Ray Spectrometer on the Solar Maximum Mission satellite already imply a bound on the coupling $g < 3 \times 10^{-12}$ GeV$^{-1}$. The improved generation of satellite-borne detectors, like EGRET or the project GLAST, could be able to detect a pseudoscalar-to-photon signal from a nearby supernova, for allowed values of $g$.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	A light pseudoscalar coupled to two photons would be copiously emitted by the core of a supernova.	background 0.97	0.10	0.07	asserted 0.78
s1	Part of this flux would be converted to $\gamma-$rays by the galactic magnetic field.	background 0.74	0.10	0.06	hedged possibility 0.57
s2	Measurements on the SN1987A $\gamma-$ray flux by the Gamma-Ray Spectrometer on the Solar Maximum Mission satellite already imply a bound on the coupling $g < 3 \times 10^{-12}$ GeV$^{-1}$.	result 0.73	0.17	0.72	asserted 0.90
s3	The improved generation of satellite-borne detectors, like EGRET or the project GLAST, could be able to detect a pseudoscalar-to-photon signal from a nearby supernova, for allowed values of $g$.	future work 0.88	0.09	0.22	hedged possibility 1.00

What kind of paper the classifier reports this is: theoretical result 0.89 · evidence from analysis of existing data 0.95.

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arXiv listing abstract v1

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Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

References

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Measurements on the SN1987A gamma-ray flux by the Gamma-Ray Spectrometer on the Solar Maximum Mission satellite imply stringents bounds on such process.

Pseudoscalar Conversion and Gamma-Rays from Supernovae · 0.82

Papers citing it · 56 sentences without a confident label

Uses its data or values 2 papers

Additionally, discussions on the absence of a gamma-ray flux associated with the SN1987A supernova have lead to an even more severe upper bound on their couplings to photons, which however only applies for nearly massless ALPs with $m≲10^-9$ eV: $g≲10^-11$ GeV$^-1$ [ref] or even $g≲3×10^-12$GeV$^-1$ [ref] , the most conservative one being usually used given the associated uncertainties.

Large-scale alignments of quasar polarisations: a detailed study of the spinless-particle scenario · Generic light spinless particles: searches and limits · 0.92
The lack of $γ$-ray emission from the SN1987A supernova has allowed a constraint of $≲5.3 ×10^-12$ GeV$^-1$, for $m_a ≲4.4 ×10^-10$ eV [ref] , see Fig. [ref] (although see [ref] for a recent critic).

New experimental approaches in the search for axion-like particles · Effects on photon propagation · 0.89

Compares with it 2 papers

In the case, they also lie below the upper limit derived from the nonobservation of prompt s from the supernova SN 1987a (gray shaded region) [ref] .

First lower limits on the photon-axion-like particle coupling from very high energy gamma-ray observation · Results · 0.97
We note that for light ALPs, the upper bound on the ALP-photon coupling derived here, |_B_0=31.5μG < 1.49 ×10^-12 GeV^-1 , at 95% confidence level, is a factor of $≳3$ stronger than the upper bound obtained from the analysis of SN987A [ref] .

A New Bound on Axion-Like Particles · Results · 1.00

Cites it as background 7 papers

Over the years, similar SN 1987A bounds on $g_aγ$ have been derived by several groups [ref] .

Axion-photon conversion in transient compact stars: Systematics, constraints, and opportunities · SN 1987A constraints on · 0.81
Axions can be produced in this environment through different processes, including the Primakoff process [ref] , and the electron bremsstrahlung [ref] .

Stellar Evolution confronts Axion Models · Supernovae · 0.84
A well studied example is that of light ALPs ($m_a ≲10^-10$ eV) coupled to photons, produced in the SN core through the Primakoff process and converted into gamma rays in the magnetic field of the Milky Way [ref] .

Supernova bounds on axion-like particles coupled with nucleons and electrons · Introduction · 0.82

Discussion

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