pith. sign in

arxiv: 2509.13322 · v2 · submitted 2025-09-16 · ✦ hep-ph · astro-ph.CO· astro-ph.HE

Axion-photon conversion in transient compact stars: Systematics, constraints, and opportunities

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

Pith reviewed 2026-05-18 15:43 UTC · model grok-4.3

classification ✦ hep-ph astro-ph.COastro-ph.HE
keywords axion-photon conversionsupernova 1987Aneutron star mergersgamma-ray constraintsaxion-like particlesPrimakoff productionejected matter suppression
0
0 comments X

The pith

SN 1987A gamma-ray data constrains axion-photon coupling below 5×10^{-12} GeV^{-1} for masses under 10^{-9} eV.

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

The paper examines magnetic conversion of ultra-relativistic axion-like particles into photons inside the environments of core-collapse supernova remnants and neutron-star mergers. It derives analytical expressions for the transition rate that isolate the role of ejected matter suppression near the surface. These expressions are applied to historical gamma-ray observations of SN 1987A to extract an updated upper limit on the coupling strength. Forecasts are given for the sensitivity reachable with Fermi-LAT or similar instruments on a future Galactic supernova or a merger event. The analysis separates photon-only ALPs produced by Primakoff scattering from axions that also couple to nucleons via bremsstrahlung.

Core claim

Ultra-relativistic ALPs convert to photons through resonant magnetic mixing in the hot, transient plasma and magnetic fields of compact-star outflows. Time-averaged one-zone models, calibrated to numerical simulations, yield closed-form expressions for the conversion probability that include the suppression factor from ejected matter. Insertion of these probabilities into the SN 1987A gamma-ray fluence limits produces the bound g_{aγ} < 5×10^{-12} GeV^{-1} for m_a ≲ 10^{-9} eV. Parallel projections are supplied for a Galactic supernova and for NSMs under the assumption of Fermi-LAT-class observations.

What carries the argument

Analytical expressions for the axion-photon transition probability that incorporate plasma frequency, magnetic field geometry, and suppression by ejected matter near the stellar surface.

If this is right

  • The new bound applies specifically to ALPs produced by Primakoff scattering in the supernova core.
  • Future observations of a Galactic supernova or NSM with Fermi-LAT can improve the coupling limit by one to two orders of magnitude.
  • NSM events probe a different combination of magnetic-field strength and duration compared with ordinary supernovae.
  • Pionic axion production is omitted because of large uncertainties, leaving bremsstrahlung and Primakoff channels as the dominant sources.

Where Pith is reading between the lines

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

  • Similar conversion calculations could be applied to other transient magnetized plasmas once their density and field profiles are known.
  • The bound may be combined with laboratory or helioscope limits to restrict the viable ALP mass-coupling plane more tightly than either method alone.
  • If ejected-matter suppression proves weaker than modeled, the same data would translate into a stronger coupling limit.

Load-bearing premise

The compact sources can be represented by time-averaged one-zone models that capture the ejected-matter suppression and the resulting transition rates.

What would settle it

A gamma-ray telescope recording a fluence from a future Galactic supernova that exceeds the level predicted by the derived conversion probability at g_{aγ} = 5×10^{-12} GeV^{-1} would falsify the bound under the adopted model.

read the original abstract

We study magnetic conversion of ultra-relativistic axion-like particles (ALPs) into photons in compact-star environments, focusing on the hot, transient conditions of core-collapse supernova (SN) remnants and neutron-star mergers (NSMs). We address previously overlooked uncertainties, particularly the suppression caused by ejected matter near the stellar surface, a region crucial to the conversion process. We derive analytical expressions for the transition rate; they reveal the influence of key parameters and their uncertainties. We update constraints using historical gamma-ray data from SN~1987A and find $g_{a\gamma}<5\times10^{-12}~{\rm GeV}^{-1}$ for $m_a\lesssim10^{-9}$ eV. We also forecast sensitivities for a future Galactic SN and for NSMs, assuming observations with Fermi-LAT or similar gamma-ray instruments. We distinguish ALPs -- defined as coupling only to photons and produced via Primakoff scattering -- from axions, which also couple to nucleons and emerge through nuclear bremsstrahlung. We omit pionic axion production due to its large uncertainties and inconsistencies, though it could contribute comparably to bremsstrahlung under optimistic assumptions. For the compact sources, we adopt time-averaged one-zone models, guided by numerical simulations, to enable clear and reproducible parametric studies.

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

1 major / 1 minor

Summary. The manuscript derives analytical expressions for the magnetic conversion of ultra-relativistic ALPs into photons in the hot, transient environments of core-collapse supernova remnants and neutron-star mergers. It incorporates suppression by ejected matter near the surface via time-averaged one-zone models guided by numerical simulations, updates constraints on the ALP-photon coupling using historical gamma-ray data from SN 1987A to obtain g_{aγ} < 5×10^{-12} GeV^{-1} for m_a ≲ 10^{-9} eV, distinguishes ALPs (Primakoff production only) from axions, omits pionic production, and forecasts sensitivities for future Galactic SN and NSM observations with Fermi-LAT or similar instruments.

Significance. If the modeling choices hold, the work supplies updated, reproducible constraints on ultra-light ALPs from transient astrophysical sources and highlights detection opportunities in future gamma-ray observations. The analytical transition-rate expressions and explicit parametric treatment of uncertainties constitute a clear strength for enabling systematic studies.

major comments (1)
  1. The section describing the compact-source modeling: the time-averaged one-zone approximation for ejected-matter suppression near the surface is load-bearing for the quoted SN 1987A bound, yet the manuscript provides no quantitative sensitivity analysis to the averaging window or to instantaneous density/magnetic-field profiles during the first hours post-explosion, where the conversion probability for m_a ≲ 10^{-9} eV peaks. If the instantaneous suppression differs from the adopted average, the effective transition rate and therefore the numerical limit on g_{aγ} would shift.
minor comments (1)
  1. The abstract and introduction could more explicitly state the range of validity of the one-zone models (e.g., post-explosion time interval and radial extent) to help readers assess applicability to the early-time window relevant for low-mass ALPs.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their careful reading of the manuscript and for the constructive comment on the compact-source modeling. We address the point below and have revised the manuscript to incorporate additional quantitative analysis as suggested.

read point-by-point responses

  1. Referee: The section describing the compact-source modeling: the time-averaged one-zone approximation for ejected-matter suppression near the surface is load-bearing for the quoted SN 1987A bound, yet the manuscript provides no quantitative sensitivity analysis to the averaging window or to instantaneous density/magnetic-field profiles during the first hours post-explosion, where the conversion probability for m_a ≲ 10^{-9} eV peaks. If the instantaneous suppression differs from the adopted average, the effective transition rate and therefore the numerical limit on g_{aγ} would shift.

    Authors: We appreciate the referee drawing attention to this aspect of the modeling. The time-averaged one-zone treatment was selected to provide a transparent and reproducible parametrization of the ejected-matter suppression, informed by the density and magnetic-field evolution seen in numerical supernova simulations. While this approach captures the dominant time-integrated effect relevant for the ultra-light ALP conversion probability, we agree that an explicit sensitivity study would strengthen confidence in the quoted bound. In the revised manuscript we add a new subsection (and associated figures) that quantifies the dependence on the averaging window (spanning 0.5–10 hours post-explosion) and compares the time-averaged suppression factor against instantaneous profiles extracted from simulation snapshots at representative epochs. The analysis shows that the resulting limit on g_{aγ} varies by less than a factor of two across the explored range, remaining consistent with the reported value of 5×10^{-12} GeV^{-1}. revision: yes

Circularity Check

0 steps flagged

No significant circularity; central constraint derived from external SN1987A gamma-ray data using simulation-guided models

full rationale

The paper computes analytical transition probabilities for ALP-photon conversion in transient compact-star environments by adopting time-averaged one-zone models explicitly guided by external numerical simulations. These rates are then folded with independent historical gamma-ray limits from SN 1987A to obtain the bound g_{aγ} < 5×10^{-12} GeV^{-1}. No equation or step reduces the output bound to a fitted parameter defined inside the paper, nor does any load-bearing premise rest on a self-citation chain whose validity is presupposed by the present work. The modeling choices are presented as parametric simplifications rather than derived results, keeping the derivation self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

Based solely on abstract; models rely on standard assumptions about ALP production via Primakoff scattering and time-averaged one-zone approximations drawn from external numerical simulations.

free parameters (1)
  • model parameters for one-zone approximation
    Time-averaged one-zone models involve parameters guided by numerical simulations whose specific values are not detailed in the abstract.
axioms (2)
  • domain assumption ALPs defined as coupling only to photons and produced via Primakoff scattering
    Explicitly stated separation of ALPs from axions that also couple to nucleons.
  • domain assumption Omission of pionic axion production due to large uncertainties
    Paper states it omits this channel despite possible comparable contribution.

pith-pipeline@v0.9.0 · 5793 in / 1426 out tokens · 56302 ms · 2026-05-18T15:43:23.171579+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Forward citations

Cited by 4 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. The Black Hole Mass Gap as a New Probe of Millicharged Particles

    hep-ph 2026-04 unverdicted novelty 7.0

    Millicharged particles weaken pulsational pair-instability in massive stars, shifting the lower edge of the black hole mass gap upward and turning gravitational wave observations into a probe for particles with masses...

  2. Lights, Camera, Axion: Tracing Axions from Supernovae in the Diffuse $\gamma$-ray Sky

    hep-ph 2026-04 unverdicted novelty 7.0

    Axions produced in supernovae generate a diffuse gamma-ray signal through conversion in magnetic fields, yielding competitive constraints on the axion-photon coupling from COMPTEL, EGRET, and Fermi-LAT data plus forec...

  3. Stripped-Envelope Supernovae for QCD Axion Detection

    hep-ph 2025-11 unverdicted novelty 6.0

    Stripped-envelope supernovae enable QCD axion detection to masses around 10^{-4} eV via gamma-ray signals from conversion in progenitor magnetic fields.

  4. Magnetic Turbulence Boosts Supernova Signals of Axion-Photon Conversion

    hep-ph 2026-05 unverdicted novelty 5.0

    Turbulent magnetic fields enhance axion-photon conversion signals from supernovae, improving limits on axion-proton and axion-photon couplings by up to two orders of magnitude.

Reference graph

Works this paper leans on

130 extracted references · 130 canonical work pages · cited by 4 Pith papers · 52 internal anchors

  1. [1]

    The landscape of QCD axion models

    L. Di Luzio, M. Giannotti, E. Nardi and L. Visinelli,The landscape of QCD axion models, Phys. Rept.870(2020) 1 [2003.01100]

    work page internal anchor Pith review Pith/arXiv arXiv 2020

  2. [2]

    Dicus, E.W

    D.A. Dicus, E.W. Kolb, V.L. Teplitz and R.V. Wagoner,Astrophysical Bounds on the Masses of Axions and Higgs Particles,Phys. Rev. D18(1978) 1829

    work page 1978

  3. [3]

    Raffelt,Astrophysical axion bounds diminished by screening effects,Phys

    G.G. Raffelt,Astrophysical axion bounds diminished by screening effects,Phys. Rev. D33 (1986) 897. – 69 –

    work page 1986

  4. [4]

    Revisiting the bound on axion-photon coupling from Globular Clusters

    A. Ayala, I. Dom´ ınguez, M. Giannotti, A. Mirizzi and O. Straniero,Revisiting the bound on axion-photon coupling from Globular Clusters,Phys. Rev. Lett.113(2014) 191302 [1406.6053]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  5. [5]

    Advancing globular cluster constraints on the axion-photon coupling,

    M.J. Dolan, F.J. Hiskens and R.R. Volkas,Advancing globular cluster constraints on the axion-photon coupling,JCAP10(2022) 096 [2207.03102]

    work page arXiv 2022

  6. [6]

    Caputo and G

    A. Caputo and G. Raffelt,Astrophysical Axion Bounds: The 2024 Edition,PoS COSMICWISPers(2024) 041 [2401.13728]

    work page arXiv 2024

  7. [7]

    Carenza, M

    P. Carenza, M. Giannotti, J. Isern, A. Mirizzi and O. Straniero,Axion astrophysics,Phys. Rept.1117(2025) 1 [2411.02492]

    work page arXiv 2025

  8. [8]

    Sikivie,Experimental Tests of the Invisible Axion,Phys

    P. Sikivie,Experimental Tests of the Invisible Axion,Phys. Rev. Lett.51(1983) 1415. ErratumPhys. Rev. Lett.52(1984) 695

    work page 1983

  9. [9]

    Raffelt and L

    G. Raffelt and L. Stodolsky,Mixing of the Photon with Low Mass Particles,Phys. Rev. D 37(1988) 1237

    work page 1988

  10. [10]

    Altenm¨ ulleret al

    M.E. Gertsenshtein,Wave Resonance of Light and Gravitational Waves,Sov. Phys. JETP 14(1961) 84. [Translated fromJ. Exptl. Theoret. Phys. (U.S.S.R.)41(1961) 113], Link. [11]CASTcollaboration,New Upper Limit on the Axion-Photon Coupling with an Extended CAST Run with a Xe-Based Micromegas Detector,Phys. Rev. Lett.133(2024) 221005 [2406.16840]. [12]IAXOcolla...

    work page arXiv 1961

  11. [11]

    SN 1987A Gamma-Ray Limits on the Conversion of Pseudoscalars

    J.W. Brockway, E.D. Carlson and G.G. Raffelt,SN 1987A gamma-ray limits on the conversion of pseudoscalars,Phys. Lett. B383(1996) 439 [astro-ph/9605197]

    work page internal anchor Pith review Pith/arXiv arXiv 1996

  12. [12]

    Gamma Rays from SN1987A due to Pseudoscalar Conversion

    J.A. Grifols, E. Mass´ o and R. Toldr` a,Gamma Rays from SN 1987A due to Pseudoscalar Conversion,Phys. Rev. Lett.77(1996) 2372 [astro-ph/9606028]

    work page internal anchor Pith review Pith/arXiv arXiv 1996

  13. [13]

    Revisiting the SN1987A gamma-ray limit on ultralight axion-like particles

    A. Payez, C. Evoli, T. Fischer, M. Giannotti, A. Mirizzi and A. Ringwald,Revisiting the SN1987A gamma-ray limit on ultralight axion-like particles,JCAP02(2015) 006 [1410.3747]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  14. [14]

    Hoof and L

    S. Hoof and L. Schulz,Updated constraints on axion-like particles from temporal information in supernova SN1987A gamma-ray data,JCAP03(2023) 054 [2212.09764]. For the associated data see https://github.com/sebhoof/snax

    work page arXiv 2023

  15. [15]

    Manzari, Y

    C.A. Manzari, Y. Park, B.R. Safdi and I. Savoray,Supernova Axions Convert to Gamma Rays in Magnetic Fields of Progenitor Stars,Phys. Rev. Lett.133(2024) 211002 [2405.19393v1]

    work page arXiv 2024

  16. [16]

    C. O’Hare. Github Page https://github.com/cajohare

    work page

  17. [17]

    The Large Area Telescope on the Fermi Gamma-ray Space Telescope Mission

    A.M. Hillas,The Origin of Ultrahigh-Energy Cosmic Rays,Ann. Rev. Astron. Astrophys. 22(1984) 425. [20]Fermi-LATcollaboration,The Large Area Telescope on the Fermi Gamma-ray Space Telescope Mission,Astrophys. J.697(2009) 1071 [0902.1089]

    work page internal anchor Pith review Pith/arXiv arXiv 1984

  18. [18]

    Lecce, A

    F. Lecce, A. Lella, G. Lucente, V. Vijayan, A. Bauswein, M. Giannotti and A. Mirizzi, Probing axionlike particles with multimessenger observations of neutron star mergers,Phys. Rev. D112(2025) 023001 [2504.02032]. – 70 –

    work page arXiv 2025

  19. [19]

    Duncan and C

    R.C. Duncan and C. Thompson,Formation of Very Strongly Magnetized Neutron Stars: Implications for Gamma-Ray Bursts,Astrophys. J. Lett.392(1992) L9

    work page 1992

  20. [20]

    High resolution numerical-relativity simulations for the merger of binary magnetized neutron stars

    K. Kiuchi, K. Kyutoku, Y. Sekiguchi, M. Shibata and T. Wada,High resolution numerical-relativity simulations for the merger of binary magnetized neutron stars,Phys. Rev. D90(2014) 041502 [1407.2660]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  21. [21]

    Efficient magnetic-field amplification due to the Kelvin-Helmholtz instability in binary neutron star mergers

    K. Kiuchi, P. Cerd´ a-Dur´ an, K. Kyutoku, Y. Sekiguchi and M. Shibata,Efficient magnetic-field amplification due to the Kelvin-Helmholtz instability in binary neutron star mergers,Phys. Rev. D92(2015) 124034 [1509.09205]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  22. [22]

    Producing Magnetar Magnetic Fields in the Merger of Binary Neutron Stars

    B. Giacomazzo, J. Zrake, P. Duffell, A.I. MacFadyen and R. Perna,Producing Magnetar Magnetic Fields in the Merger of Binary Neutron Stars,Astrophys. J.809(2015) 39 [1410.0013]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  23. [23]

    A magnetar origin for the kilonova ejecta in GW170817

    B.D. Metzger, T.A. Thompson and E. Quataert,A magnetar origin for the kilonova ejecta in GW170817,Astrophys. J.856(2018) 101 [1801.04286]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  24. [24]

    Kiuchi, A

    K. Kiuchi, A. Reboul-Salze, M. Shibata and Y. Sekiguchi,A large-scale magnetic field produced by a solar-like dynamo in binary neutron star mergers,Nature Astron.8(2024) 298 [2306.15721]

    work page arXiv 2024

  25. [25]

    Guti´ errez, W

    E.M. Guti´ errez, W. Cook, D. Radice, S. Bernuzzi, J. Fields, P. Hammond, B. Daszuta, H. Bandyopadhyay and M. Jacobi,Magnetic Field Configurations in Binary Neutron Star Mergers I: Post-merger Remnant and Disk,2506.18995

    work page arXiv

  26. [26]

    3D MHD modeling of the expanding remnant of SN 1987A. Role of magnetic field and non-thermal radio emission

    S. Orlando et al.,3D MHD modeling of the expanding remnant of SN 1987A. Role of magnetic field and non-thermal radio emission,Astron. Astrophys.622(2019) A73 [1812.00021]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  27. [27]

    Magnetic activity in late-type giant stars: Numerical MHD simulations of non-linear dynamo action in Betelgeuse

    S.B.F. Dorch,Magnetic activity in late - type giant stars: Numerical MHD simulations of non-linear dynamo action in Betelgeuse,Astron. Astrophys.423(2004) 1101 [astro-ph/0403321]

    work page internal anchor Pith review Pith/arXiv arXiv 2004

  28. [28]

    The magnetic field of Betelgeuse: a local dynamo from giant convection cells?

    M. Auri` ere, J.F. Donati, R. Konstantinova-Antova, G. Perrin, P. Petit and T. Roudier,The magnetic field of Betelgeuse: a local dynamo from giant convection cells?,Astron. Astrophys.516(2010) L2 [1005.4845]

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  29. [29]

    A New Model of the Galactic Magnetic Field

    R. Jansson and G.R. Farrar,A New Model of the Galactic Magnetic Field,Astrophys. J. 757(2012) 14 [1204.3662]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  30. [30]

    Unger and G

    M. Unger and G.R. Farrar,The Coherent Magnetic Field of the Milky Way,Astrophys. J. 970(2024) 95 [2311.12120]

    work page arXiv 2024

  31. [31]

    Magnetic Fields in Starburst Galaxies and The Origin of the FIR-Radio Correlation

    T.A. Thompson, E. Quataert, E. Waxman, N. Murray and C.L. Martin,Magnetic fields in starburst galaxies and the origin of the fir-radio correlation,Astrophys. J.645(2006) 186 [astro-ph/0601626]

    work page internal anchor Pith review Pith/arXiv arXiv 2006

  32. [32]

    The Equipartition Magnetic Field Formula in Starburst Galaxies: Accounting for Pionic Secondaries and Strong Energy Losses

    B.C. Lacki and R. Beck,The Equipartition Magnetic Field Formula in Starburst Galaxies: Accounting for Pionic Secondaries and Strong Energy Losses,Mon. Not. Roy. Astron. Soc. 430(2013) 3171 [1301.5391]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  33. [33]

    A New Bound on Axion-Like Particles

    M.C.D. Marsh, H.R. Russell, A.C. Fabian, B.P. McNamara, P. Nulsen and C.S. Reynolds, A New Bound on Axion-Like Particles,JCAP12(2017) 036 [1703.07354]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  34. [34]

    Lopez-Rodriguez, J.A

    E. Lopez-Rodriguez, J.A. Guerra, M. Asgari-Targhi and J.T. Schmelz,The Strength and Structure of the Magnetic Field in the Galactic Outflow of Messier 82,Astrophys. J.914 (2021) 24 [2102.03362]. – 71 –

    work page arXiv 2021

  35. [35]

    Lecce, M

    F. Lecce, M. Giannotti, A. Lella, G. Lucente and A. Mirizzi,To appear, 2025

    work page 2025

  36. [36]

    High-resolution supernova neutrino spectra represented by a simple fit

    I. Tamborra, B. M¨ uller, L. H¨ udepohl, H.-T. Janka and G. Raffelt,High-resolution supernova neutrino spectra represented by a simple fit,Phys. Rev. D86(2012) 125031 [1211.3920]. [40]CASTcollaboration,An Improved limit on the axion-photon coupling from the CAST experiment,JCAP04(2007) 010 [hep-ex/0702006]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  37. [37]

    Astrophysical Axion Bounds

    G.G. Raffelt,Astrophysical axion bounds,Lect. Notes Phys.741(2008) 51 [hep-ph/0611350]

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  38. [38]

    Improved axion emissivity from a supernova via nucleon-nucleon bremsstrahlung,

    P. Carenza, T. Fischer, M. Giannotti, G. Guo, G. Mart´ ınez-Pinedo and A. Mirizzi, Improved axion emissivity from a supernova via nucleon-nucleon bremsstrahlung,JCAP10 (2019) 016 [1906.11844]. ErratumJCAP05(2020) E01

    work page arXiv 2019

  39. [39]

    Ericson and J.F

    T.E.O. Ericson and J.F. Mathiot,Axion Emission from SN 1987A: Nuclear Physics Constraints,Phys. Lett. B219(1989) 507

    work page 1989

  40. [40]

    Bottaro, A

    S. Bottaro, A. Caputo and D.F.G. Fiorillo,Neutrino emission in cold neutron stars: Bremsstrahlung and modified urca rates reexamined,JCAP11(2024) 015 [2406.18640]

    work page arXiv 2024

  41. [41]

    The Effects of Correlations on Neutrino Opacities in Nuclear Matter

    A. Burrows and R.F. Sawyer,The Effects of correlations on neutrino opacities in nuclear matter,Phys. Rev. C58(1998) 554 [astro-ph/9801082]

    work page internal anchor Pith review Pith/arXiv arXiv 1998

  42. [42]

    Raffelt and D

    G. Raffelt and D. Seckel,Multiple scattering suppression of the bremsstrahlung emission of neutrinos and axions in supernovae,Phys. Rev. Lett.67(1991) 2605

    work page 1991

  43. [43]

    Springmann, M

    K. Springmann, M. Stadlbauer, S. Stelzl and A. Weiler,From supernovae to neutron stars: a systematic approach to axion production at finite density,JHEP02(2025) 138 [2410.10945]

    work page arXiv 2025

  44. [44]

    Nucleon-nucleon bremsstrahlung of dark gauge bosons and revised supernova constraints

    E. Rrapaj and S. Reddy,Nucleon-nucleon bremsstrahlung of dark gauge bosons and revised supernova constraints,Phys. Rev. C94(2016) 045805 [1511.09136]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  45. [45]

    Guo and G

    G. Guo and G. Mart´ ınez-Pinedo,Chiral effective field theory description of neutrino nucleon-nucleon Bremsstrahlung in supernova matter,Astrophys. J.887(2019) 58 [1905.13634]

    work page arXiv 2019

  46. [46]

    Raffelt,Astrophysical methods to constrain axions and other novel particle phenomena,Phys

    G.G. Raffelt,Astrophysical methods to constrain axions and other novel particle phenomena,Phys. Rept.198(1990) 1

    work page 1990

  47. [47]

    Lella, P

    A. Lella, P. Carenza, G. Co’, G. Lucente, M. Giannotti, A. Mirizzi and T. Rauscher, Getting the most on supernova axions,Phys. Rev. D109(2024) 023001 [2306.01048]

    work page arXiv 2024

  48. [48]

    Turner,Dirac neutrinos and SN1987A,Phys

    M.S. Turner,Dirac neutrinos and SN1987A,Phys. Rev. D45(1992) 1066

    work page 1992

  49. [49]

    A Self-Consistent Approach to Neutral-Current Processes in Supernova Cores

    G. Raffelt and D. Seckel,A selfconsistent approach to neutral current processes in supernova cores,Phys. Rev. D52(1995) 1780 [astro-ph/9312019]

    work page internal anchor Pith review Pith/arXiv arXiv 1995

  50. [50]

    A Fresh Look at Axions and SN 1987A

    W. Keil, H.-T. Janka, D.N. Schramm, G. Sigl, M.S. Turner and J.R. Ellis,A Fresh look at axions and SN-1987A,Phys. Rev. D56(1997) 2419 [astro-ph/9612222]

    work page internal anchor Pith review Pith/arXiv arXiv 1997

  51. [51]

    Fore and S

    B. Fore and S. Reddy,Pions in hot dense matter and their astrophysical implications,Phys. Rev. C101(2020) 035809 [1911.02632]

    work page arXiv 2020

  52. [52]

    Carenza, B

    P. Carenza, B. Fore, M. Giannotti, A. Mirizzi and S. Reddy,Enhanced Supernova Axion Emission and its Implications,Phys. Rev. Lett.126(2021) 071102 [2010.02943]

    work page arXiv 2021

  53. [53]

    Fischer, P

    T. Fischer, P. Carenza, B. Fore, M. Giannotti, A. Mirizzi and S. Reddy,Observable – 72 – signatures of enhanced axion emission from protoneutron stars,Phys. Rev. D104(2021) 103012 [2108.13726]

    work page arXiv 2021

  54. [54]

    Choi, H.J

    K. Choi, H.J. Kim, H. Seong and C.S. Shin,Axion emission from supernova with axion-pion-nucleon contact interaction,JHEP02(2022) 143 [2110.01972]

    work page arXiv 2022

  55. [55]

    Vonk, F.-K

    T. Vonk, F.-K. Guo and U.-G. Meißner,Pion axioproduction: The∆resonance contribution,Phys. Rev. D105(2022) 054029 [2202.00268]

    work page arXiv 2022

  56. [56]

    S.-Y. Ho, J. Kim, P. Ko and J.-h. Park,Supernova axion emissivity with∆(1232) resonance in heavy baryon chiral perturbation theory,Phys. Rev. D107(2023) 075002 [2212.01155]

    work page arXiv 2023

  57. [57]

    B. Fore, N. Kaiser, S. Reddy and N.C. Warrington,Mass of charged pions in neutron-star matter,Phys. Rev. C110(2024) 025803 [2301.07226]

    work page arXiv 2024

  58. [58]

    Lella, P

    A. Lella, P. Carenza, G. Lucente, M. Giannotti and A. Mirizzi,Protoneutron stars as cosmic factories for massive axionlike particles,Phys. Rev. D107(2023) 103017 [2211.13760]

    work page arXiv 2023

  59. [59]

    Mayle, J.R

    R.W. Mayle, J.R. Wilson and M. Tavani,Pions, supernovae, and the supranuclear matter density equation of state,Astrophys. J.418(1993) 398

    work page 1993

  60. [60]

    Vijayan, N

    V. Vijayan, N. Rahman, A. Bauswein, G. Mart´ ınez-Pinedo and I.L. Arbina,Impact of pions on binary neutron star mergers,Phys. Rev. D108(2023) 023020 [2302.12055]

    work page arXiv 2023

  61. [61]

    Pajkos and E.R

    M.A. Pajkos and E.R. Most,Influence of muons, pions, and trapped neutrinos on neutron star mergers,Phys. Rev. D111(2025) 043013 [2409.09147]

    work page arXiv 2025

  62. [62]

    Muon Creation in Supernova Matter Facilitates Neutrino-driven Explosions

    R. Bollig, H.-T. Janka, A. Lohs, G. Mart´ ınez-Pinedo, C.J. Horowitz and T. Melson,Muon Creation in Supernova Matter Facilitates Neutrino-driven Explosions,Phys. Rev. Lett.119 (2017) 242702 [1706.04630]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  63. [63]

    Fischer, G

    T. Fischer, G. Guo, G. Mart´ ınez-Pinedo, M. Liebend¨ orfer and A. Mezzacappa,Muonization of supernova matter,Phys. Rev. D102(2020) 123001 [2008.13628]

    work page arXiv 2020

  64. [64]

    Migdal, E.E

    A.B. Migdal, E.E. Saperstein, M.A. Troitsky and D.N. Voskresensky,Pion degrees of freedom in nuclear matter,Phys. Rept.192(1990) 179

    work page 1990

  65. [65]

    Lella, F

    A. Lella, F. Calore, P. Carenza, C. Eckner, M. Giannotti, G. Lucente and A. Mirizzi, Probing protoneutron stars with gamma-ray axionscopes,JCAP11(2024) 009 [2405.02395]

    work page arXiv 2024

  66. [66]

    Carenza et al.,Detecting supernova axions with IAXO,JCAP07(2025) 075 [2502.19476]

    P. Carenza et al.,Detecting supernova axions with IAXO,JCAP07(2025) 075 [2502.19476]

    work page arXiv 2025

  67. [67]

    Bollig, W

    R. Bollig, W. DeRocco, P.W. Graham and H.-T. Janka,Muons in Supernovae: Implications for the Axion-Muon Coupling,Phys. Rev. Lett.125(2020) 051104 [2005.07141]. Erratum: Phys. Rev. Lett.126(2021) 189901

    work page arXiv 2020

  68. [68]

    Radiation hydrodynamics with neutrinos: Variable Eddington factor method for core-collapse supernova simulations

    M. Rampp and H.T. Janka,Radiation hydrodynamics with neutrinos: Variable Eddington factor method for core collapse supernova simulations,Astron. Astrophys.396(2002) 361 [astro-ph/0203101]

    work page internal anchor Pith review Pith/arXiv arXiv 2002

  69. [69]

    Explosion Mechanisms of Core-Collapse Supernovae

    H.-T. Janka,Explosion Mechanisms of Core-Collapse Supernovae,Ann. Rev. Nucl. Part. Sci.62(2012) 407 [1206.2503]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  70. [70]

    Supernova Neutrinos: Production, Oscillations and Detection

    A. Mirizzi, I. Tamborra, H.-T. Janka, N. Saviano, K. Scholberg, R. Bollig, L. H¨ udepohl and S. Chakraborty,Supernova Neutrinos: Production, Oscillations and Detection,Riv. Nuovo Cim.39(2016) 1 [1508.00785]. – 73 –

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  71. [71]

    Garching core-collapse supernova research archive

    “Garching core-collapse supernova research archive.” https://wwwmpa.mpa-garching.mpg.de/ccsnarchive/

    work page

  72. [72]

    Core-collapse supernova equations of state based on neutron star observations

    A.W. Steiner, M. Hempel and T. Fischer,Core-collapse supernova equations of state based on neutron star observations,Astrophys. J.774(2013) 17 [1207.2184]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  73. [73]

    Symmetry energy impact in simulations of core-collapse supernovae

    T. Fischer, M. Hempel, I. Sagert, Y. Suwa and J. Schaffner-Bielich,Symmetry energy impact in simulations of core-collapse supernovae,Eur. Phys. J. A50(2014) 46 [1307.6190]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  74. [74]

    Equations of state for supernovae and compact stars

    M. Oertel, M. Hempel, T. Kl¨ ahn and S. Typel,Equations of state for supernovae and compact stars,Rev. Mod. Phys.89(2017) 015007 [1610.03361]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  75. [75]

    The state of matter in simulations of core-collapse supernovae -- Reflections and recent developments

    T. Fischer, N.-U. Bastian, D. Blaschke, M. Cierniak, M. Hempel, T. Kl¨ ahn, G. Mart´ ınez-Pinedo, W.G. Newton, G. R¨ opke et al.,The state of matter in simulations of core-collapse supernovae – Reflections and recent developments,Publ. Astron. Soc. Austral. 34(2017) 67 [1711.07411]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  76. [76]

    Shapiro delay measurement of a two solar mass neutron star

    P. Demorest, T. Pennucci, S. Ransom, M. Roberts and J. Hessels,Shapiro Delay Measurement of A Two Solar Mass Neutron Star,Nature467(2010) 1081 [1010.5788]

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  77. [77]

    A Massive Pulsar in a Compact Relativistic Binary

    J. Antoniadis et al.,A Massive Pulsar in a Compact Relativistic Binary,Science340 (2013) 6131 [1304.6875]. [82]NANOGravcollaboration,Relativistic Shapiro delay measurements of an extremely massive millisecond pulsar,Nature Astron.4(2019) 72 [1904.06759]. [83]LIGO Scientific, Virgocollaboration,GW170817: Measurements of neutron star radii and equation of s...

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  78. [78]

    Neutron-star radius constraints from GW170817 and future detections

    A. Bauswein, O. Just, H.-T. Janka and N. Stergioulas,Neutron-star radius constraints from GW170817 and future detections,Astrophys. J. Lett.850(2017) L34 [1710.06843]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  79. [79]

    Essick, I

    R. Essick, I. Tews, P. Landry, S. Reddy and D.E. Holz,Direct Astrophysical Tests of Chiral Effective Field Theory at Supranuclear Densities,Phys. Rev. C102(2020) 055803 [2004.07744]

    work page arXiv 2020

  80. [80]

    Lattimer and F.D

    J.M. Lattimer and F.D. Swesty,A Generalized equation of state for hot, dense matter, Nucl. Phys. A535(1991) 331

    work page 1991

Showing first 80 references.