arxiv: 2512.13816 · v2 · submitted 2025-12-15 · ✦ hep-ph · astro-ph.HE· astro-ph.SR· gr-qc

Recognition: 1 theorem link

· Lean Theorem

Stellar Superradiance and Low-Energy Absorption in Dense Nuclear Media

Zhaoyu Bai , Vitor Cardoso , Yifan Chen , Yuyan Li , Jamie I. McDonald , Hyeonseok Seong

Authors on Pith no claims yet

Pith reviewed 2026-05-16 21:39 UTC · model grok-4.3

classification ✦ hep-ph astro-ph.HEastro-ph.SRgr-qc

keywords superradianceneutron starsultralight bosonsaxionsmultiple scatteringabsorption ratesdense nuclear mattervector bosons

0 comments

The pith

Collective multiple scattering in nuclear matter strongly suppresses the low-energy absorption rate for superradiant bosonic modes around neutron stars.

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

The paper re-examines the link between microphysical boson-nucleon interactions and macroscopic superradiance in neutron stars. Previous estimates extrapolated thermal absorption rates directly to long-wavelength bound states, predicting growth rates on pulsar spindown timescales, especially for vector fields. Accounting for repeated nucleon collisions in dense matter alters the effective absorption at low energies, producing strong suppression of the superradiant rate. This changes the expected connection between stellar cooling bounds and superradiance constraints.

Core claim

A naive extrapolation of the microphysical neutron-nucleon scattering and inverse-bremsstrahlung absorption rates to the superradiant regime would imply superradiant rates comparable to astrophysical timescales characterised by pulsar spindown. However, collective multiple-scattering effects in dense nuclear matter modify the effective low-energy absorption experienced by the bosonic bound state, strongly suppressing the rate relevant for superradiance.

What carries the argument

The collective multiple-scattering correction arising from repeated nucleon collisions, which modifies the effective absorption experienced by long-wavelength bosonic bound states.

If this is right

Superradiant instability timescales for neutron stars become much longer than pulsar spindown times.
Vector boson superradiance is suppressed more strongly than scalar boson superradiance.
The link between stellar cooling constraints and superradiance bounds is weakened, with the former remaining unaffected.
Bosonic emission rates at thermal wavelengths stay the same while macroscopic bound-state growth is reduced.

Where Pith is reading between the lines

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

Similar wavelength-dependent suppression could appear in other dense media where mean free paths are short compared to mode sizes.
Refined superradiance calculations should incorporate radial density variations to test the robustness of the suppression.
The result suggests that effective absorption cross sections for bosons depend on the ratio of wavelength to nucleon collision length.
This mechanism might reduce the reach of superradiance searches for certain ultralight boson models.

Load-bearing premise

The collective multiple-scattering correction derived for thermal emission applies directly to macroscopic, long-wavelength superradiant bound states without additional kinematic or density-profile corrections that would alter the suppression factor.

What would settle it

A detailed mode calculation that includes the neutron star's density profile and shows the suppression factor changing by an order of magnitude or more for wavelengths comparable to the star's size would falsify the direct applicability of the correction.

read the original abstract

Ultralight bosons such as axions and dark photons are well-motivated hypothetical particles, whose couplings to ordinary matter can be effectively constrained by stellar cooling. Limits on these interactions can be obtained by demanding that their emission from the stellar interior does not lead to excessive energy loss. An intriguing question is whether the same microphysical couplings can also be probed through neutron star superradiance, in which gravitationally bound bosonic modes grow exponentially by extracting rotational energy from the star. Although both processes originate from boson-matter interactions, they probe very different kinematic regimes. Stellar cooling probes boson emission at thermal wavelengths, while superradiance is governed by modes whose wavelength is comparable to or greater than the size of the star. Previous work has attempted to relate the microphysical neutron-nucleon scattering and inverse-bremsstrahlung absorption rates directly to the macroscopic growth rate of superradiant bound states. In this work, we re-examine this connection and show that a naive extrapolation of the microphysical absorption rate to the superradiant regime would imply superradiant rates comparable to astrophysical timescales characterised by pulsar spindown. These naive rates are especially high for vector fields. However, we demonstrate that this conclusion changes once collective multiple-scattering effects in dense nuclear matter are taken into account. Repeated nucleon collisions modify the effective low-energy absorption experienced by the bosonic bound state, strongly suppressing the rate relevant for superradiance.

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

The paper flags that collective multiple scattering suppresses superradiant absorption rates in neutron stars, but the transfer from thermal to long-wavelength regimes is the part that needs checking.

read the letter

The main point is that naive use of microphysical absorption rates overestimates superradiant growth in neutron stars, and collective nucleon scattering in dense matter suppresses the effective low-energy rate enough to change the picture. The authors contrast the short-wavelength thermal regime of stellar cooling with the macroscopic wavelengths of superradiant modes and argue that repeated collisions modify the absorption experienced by the bound state, leading to much slower instabilities than prior extrapolations suggested, especially for vectors. This is a straightforward extension of standard nuclear-physics multiple-scattering ideas to a new context, and it is useful for anyone who has been applying direct microphysical rates to superradiance bounds on axions or dark photons. The abstract is clear that the suppression is large enough to bring the rates below typical pulsar spindown timescales. What the paper does well is to make the kinematic mismatch explicit rather than glossing over it. The argument stays within existing nuclear-physics tools and does not introduce free parameters or circular fits. The soft spot is exactly the one raised in the stress-test note: whether the suppression factor derived for local thermal scattering carries over unchanged to coherent, long-wavelength modes where k approaches zero and the field varies slowly across the stellar density profile. If the underlying multiple-scattering calculation assumes momentum transfers set by temperature or short coherence lengths, additional corrections could appear in the superradiant limit. The abstract claims the demonstration but does not show the derivation or any numerical checks, so the quantitative size of the suppression remains unverified from what is available. This work is for people who set or use astrophysical limits on ultralight bosons. A reader updating superradiance constraints would want to see whether the correction holds. It shows honest engagement with the regime difference and the literature, so it deserves a serious referee to examine the calculation details and the kinematic matching. I would send it to peer review.

Referee Report

2 major / 2 minor

Summary. The manuscript re-examines the connection between microphysical boson-nucleon absorption rates (relevant for stellar cooling constraints on ultralight bosons) and the exponential growth rates of gravitationally bound superradiant modes around neutron stars. It argues that a naive extrapolation of these rates yields superradiant timescales comparable to pulsar spindown (particularly for vector fields), but that collective multiple-scattering effects arising from repeated nucleon collisions in dense nuclear matter strongly suppress the effective low-energy absorption experienced by the long-wavelength superradiant bound states.

Significance. If the suppression is quantitatively robust, the result would indicate that neutron-star superradiance provides weaker constraints on ultralight bosons than previously estimated from direct microphysical extrapolations. The work usefully distinguishes the kinematic regimes of thermal emission versus coherent macroscopic modes and underscores the necessity of collective nuclear-physics corrections when applying low-energy rates to stellar-scale phenomena.

major comments (2)

[§4] §4 (application of multiple-scattering formalism): the suppression factor is transferred from the thermal-emission calculation (local momentum transfers ~T) to the superradiant regime (k→0, coherent over the stellar density profile) without an explicit derivation showing that the underlying assumptions on scattering locality and kinematics remain valid. This step is load-bearing for the central claim that the rate is 'strongly suppressed'.
[Eq. (18)] Eq. (18) and surrounding text: the naive absorption rate is stated to produce astrophysical timescales, yet the manuscript provides no direct numerical comparison (e.g., ratio or plot) of the suppressed versus unsuppressed rates for representative boson masses and couplings, leaving the magnitude of the effect difficult to assess.

minor comments (2)

[Abstract] The abstract and introduction would benefit from a single numerical estimate of the suppression factor (e.g., order-of-magnitude reduction) to make the change in conclusion immediately quantitative for readers.
[Notation] Notation for the microphysical versus effective absorption coefficients is introduced inconsistently; a dedicated table or equation defining the symbols would improve clarity.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading and constructive comments on our manuscript. We address each major point below and have revised the text accordingly to strengthen the presentation.

read point-by-point responses

Referee: §4 (application of multiple-scattering formalism): the suppression factor is transferred from the thermal-emission calculation (local momentum transfers ~T) to the superradiant regime (k→0, coherent over the stellar density profile) without an explicit derivation showing that the underlying assumptions on scattering locality and kinematics remain valid. This step is load-bearing for the central claim that the rate is 'strongly suppressed'.

Authors: We agree that an explicit derivation strengthens the argument. In the revised manuscript we have added a dedicated paragraph in §4 (and a short appendix) that derives the effective absorption coefficient in the long-wavelength limit directly from the multiple-scattering expansion. The derivation shows that the suppression factor depends on the ratio of the boson wavelength to the nucleon mean free path; because the relevant momentum transfers remain set by the local Fermi momentum (independent of the boson wave-vector k), the same kinematic assumptions used for thermal emission carry over to the k→0 superradiant case. The coherence of the bound state over the stellar profile is accounted for by integrating the locally suppressed rate over the density distribution. revision: yes
Referee: Eq. (18) and surrounding text: the naive absorption rate is stated to produce astrophysical timescales, yet the manuscript provides no direct numerical comparison (e.g., ratio or plot) of the suppressed versus unsuppressed rates for representative boson masses and couplings, leaving the magnitude of the effect difficult to assess.

Authors: We thank the referee for this observation. The revised manuscript now includes a new figure (Fig. 5) that directly compares the superradiant growth timescale versus boson mass for both the naive and collectively suppressed rates. Separate curves are shown for scalar and vector fields at representative couplings (g=10^{-12} and 10^{-10}). The plot demonstrates that the suppression increases the timescale by 2–5 orders of magnitude across the mass range 10^{-13}–10^{-10} eV, rendering the superradiant instability slower than typical pulsar spindown for most parameter choices. revision: yes

Circularity Check

0 steps flagged

No significant circularity detected

full rationale

The paper derives its central suppression of superradiant absorption rates by invoking collective multiple-scattering corrections in dense nuclear matter, drawn from established nuclear-physics treatments of thermal emission. No equation in the provided derivation chain reduces the claimed suppression factor to a parameter fitted inside the paper, nor does any load-bearing step collapse to a self-citation whose content is itself unverified or defined by the present work. The argument applies standard multiple-scattering ideas to a new kinematic regime without renaming known results or smuggling ansatzes via self-citation, rendering the derivation self-contained against external nuclear-matter benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claim rests on standard assumptions about boson-nucleon interactions and nuclear matter; no new free parameters, axioms, or invented entities are introduced in the abstract.

axioms (2)

domain assumption Boson emission and absorption rates in stellar interiors are governed by the same microphysical couplings as those relevant for superradiant bound states.
Invoked when contrasting stellar cooling and superradiance kinematic regimes.
domain assumption Collective multiple-scattering effects in dense nuclear matter can be modeled to modify the effective absorption at long wavelengths.
Central to the suppression argument.

pith-pipeline@v0.9.0 · 5588 in / 1474 out tokens · 40740 ms · 2026-05-16T21:39:50.246750+00:00 · methodology

discussion (0)

Reference graph

Works this paper leans on

147 extracted references · 147 canonical work pages · 41 internal anchors

[1]

R. D. Peccei and H. R. Quinn,CP Conservation in the Presence of Instantons,Phys. Rev. Lett.38(1977) 1440–1443

work page 1977
[2]

Weinberg,A New Light Boson?,Phys

S. Weinberg,A New Light Boson?,Phys. Rev. Lett.40(1978) 223–226. – 18 –

work page 1978
[3]

Wilczek,Problem of StrongPandTInvariance in the Presence of Instantons,Phys

F. Wilczek,Problem of StrongPandTInvariance in the Presence of Instantons,Phys. Rev. Lett.40(1978) 279–282

work page 1978
[4]

J. E. Kim,Weak Interaction Singlet and Strong CP Invariance,Phys. Rev. Lett.43(1979) 103

work page 1979
[5]

M. A. Shifman, A. I. Vainshtein and V. I. Zakharov,Can Confinement Ensure Natural CP Invariance of Strong Interactions?,Nucl. Phys. B166(1980) 493–506

work page 1980
[6]

M. Dine, W. Fischler and M. Srednicki,A Simple Solution to the Strong CP Problem with a Harmless Axion,Phys. Lett. B104(1981) 199–202

work page 1981
[7]

A. R. Zhitnitsky,On Possible Suppression of the Axion Hadron Interactions. (In Russian), Sov. J. Nucl. Phys.31(1980) 260

work page 1980
[8]

Preskill, M

J. Preskill, M. B. Wise and F. Wilczek,Cosmology of the Invisible Axion,Phys. Lett. B120 (1983) 127–132

work page 1983
[9]

L. F. Abbott and P. Sikivie,A Cosmological Bound on the Invisible Axion,Phys. Lett. B120 (1983) 133–136

work page 1983
[10]

Dine and W

M. Dine and W. Fischler,The Not So Harmless Axion,Phys. Lett. B120(1983) 137–141

work page 1983
[11]

Axions In String Theory

P. Svrcek and E. Witten,Axions In String Theory,JHEP06(2006) 051, [hep-th/0605206]

work page internal anchor Pith review Pith/arXiv arXiv 2006
[12]

S. A. Abel, M. D. Goodsell, J. Jaeckel, V. V. Khoze and A. Ringwald,Kinetic Mixing of the Photon with Hidden U(1)s in String Phenomenology,JHEP07(2008) 124, [0803.1449]

work page internal anchor Pith review Pith/arXiv arXiv 2008
[13]

String Axiverse

A. Arvanitaki, S. Dimopoulos, S. Dubovsky, N. Kaloper and J. March-Russell,String Axiverse,Phys. Rev. D81(2010) 123530, [0905.4720]

work page internal anchor Pith review Pith/arXiv arXiv 2010
[14]

Naturally Light Hidden Photons in LARGE Volume String Compactifications

M. Goodsell, J. Jaeckel, J. Redondo and A. Ringwald,Naturally Light Hidden Photons in LARGE Volume String Compactifications,JHEP11(2009) 027, [0909.0515]

work page internal anchor Pith review Pith/arXiv arXiv 2009
[15]

G. G. Raffelt,Stars as laboratories for fundamental physics: The astrophysics of neutrinos, axions, and other weakly interacting particles. 5, 1996

work page 1996
[16]

G. G. Raffelt,Particle physics from stars,Ann. Rev. Nucl. Part. Sci.49(1999) 163–216, [hep-ph/9903472]

work page internal anchor Pith review Pith/arXiv arXiv 1999
[17]

Caputo and G

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

work page arXiv 2024
[18]

Buschmann, C

M. Buschmann, C. Dessert, J. W. Foster, A. J. Long and B. R. Safdi,Upper Limit on the QCD Axion Mass from Isolated Neutron Star Cooling,Phys. Rev. Lett.128(2022) 091102, [2111.09892]

work page arXiv 2022
[19]

Carenza, T

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]

work page arXiv 2019
[20]

Lella, P

A. Lella, P. Carenza, G. Co’, G. Lucente, M. Giannotti, A. Mirizzi et al.,Getting the most on supernova axions,Phys. Rev. D109(2024) 023001, [2306.01048]

work page arXiv 2024
[21]

Stellar Recipes for Axion Hunters

M. Giannotti, I. G. Irastorza, J. Redondo, A. Ringwald and K. Saikawa,Stellar Recipes for Axion Hunters,JCAP10(2017) 010, [1708.02111]

work page internal anchor Pith review Pith/arXiv arXiv 2017
[22]

Capozzi and G

F. Capozzi and G. Raffelt,Axion and neutrino bounds improved with new calibrations of the tip of the red-giant branch using geometric distance determinations,Phys. Rev. D102(2020) 083007, [2007.03694]

work page arXiv 2020
[23]

Penrose and R

R. Penrose and R. M. Floyd,Extraction of rotational energy from a black hole,Nature229 (1971) 177–179

work page 1971
[24]

Y. B. Zel’Dovich,Generation of Waves by a Rotating Body,Soviet Journal of Experimental and Theoretical Physics Letters14(Aug., 1971) 180. – 19 –

work page 1971
[25]

S. L. Detweiler,KLEIN-GORDON EQUATION AND ROTATING BLACK HOLES,Phys. Rev. D22(1980) 2323–2326

work page 1980
[26]

Superradiant instabilities of rotating black branes and strings

V. Cardoso and S. Yoshida,Superradiant instabilities of rotating black branes and strings, JHEP07(2005) 009, [hep-th/0502206]

work page internal anchor Pith review Pith/arXiv arXiv 2005
[27]

S. R. Dolan,Instability of the massive Klein-Gordon field on the Kerr spacetime,Phys. Rev. D 76(2007) 084001, [0705.2880]

work page internal anchor Pith review Pith/arXiv arXiv 2007
[28]

Superradiance -- the 2020 Edition

R. Brito, V. Cardoso and P. Pani,Superradiance: New Frontiers in Black Hole Physics,Lect. Notes Phys.906(2015) pp.1–237, [1501.06570]

work page internal anchor Pith review Pith/arXiv arXiv 2015
[29]

S. Bao, Q. Xu and H. Zhang,Improved analytic solution of black hole superradiance,Phys. Rev. D106(2022) 064016, [2201.10941]

work page arXiv 2022
[30]

Exploring the String Axiverse with Precision Black Hole Physics

A. Arvanitaki and S. Dubovsky,Exploring the String Axiverse with Precision Black Hole Physics,Phys. Rev. D83(2011) 044026, [1004.3558]

work page internal anchor Pith review Pith/arXiv arXiv 2011
[31]

Bosenova collapse of axion cloud around a rotating black hole

H. Yoshino and H. Kodama,Bosenova collapse of axion cloud around a rotating black hole, Prog. Theor. Phys.128(2012) 153–190, [1203.5070]

work page internal anchor Pith review Pith/arXiv arXiv 2012
[32]

Black Hole Spindown by Light Bosons

A. Gruzinov,Black Hole Spindown by Light Bosons,1604.06422

work page internal anchor Pith review Pith/arXiv arXiv
[33]

Fukuda and K

H. Fukuda and K. Nakayama,Aspects of Nonlinear Effect on Black Hole Superradiance, JHEP01(2020) 128, [1910.06308]

work page arXiv 2020
[34]

Baryakhtar, M

M. Baryakhtar, M. Galanis, R. Lasenby and O. Simon,Black hole superradiance of self-interacting scalar fields,Phys. Rev. D103(2021) 095019, [2011.11646]

work page arXiv 2021
[35]

Omiya, T

H. Omiya, T. Takahashi and T. Tanaka,Renormalization group analysis of superradiant growth of self-interacting axion cloud,PTEP2021(2021) 043E02, [2012.03473]

work page arXiv 2021
[36]

Omiya, T

H. Omiya, T. Takahashi and T. Tanaka,Adiabatic evolution of the self-interacting axion field around rotating black holes,PTEP2022(2022) 043E03, [2201.04382]

work page arXiv 2022
[37]

Omiya, T

H. Omiya, T. Takahashi, T. Tanaka and H. Yoshino,Impact of multiple modes on the evolution of self-interacting axion condensate around rotating black holes,JCAP06(2023) 016, [2211.01949]

work page arXiv 2023
[38]

Cheng, H

L.-d. Cheng, H. Zhang and S.-s. Bao,Constraints on an axionlike particle from black hole spin superradiance,Phys. Rev. D107(2023) 063021, [2201.11338]

work page arXiv 2023
[39]

Y. Chen, X. Xue and V. Cardoso,Black holes as fermion factories,JCAP02(2025) 035, [2308.00741]

work page arXiv 2025
[40]

Y.-D. Guo, N. Jia, S.-S. Bao, H. Zhang and X. Zhang,Evolution and detection of vector superradiant instabilities,Phys. Rev. D110(2024) 083029, [2407.00767]

work page arXiv 2024
[41]

S. J. Witte and A. Mummery,Stepping up superradiance constraints on axions,Phys. Rev. D 111(2025) 083044, [2412.03655]

work page arXiv 2025
[42]

Guo, S.-S

Y.-D. Guo, S.-S. Bao, T. Li and H. Zhang,Effect of accretion on scalar superradiant instability,JCAP09(2025) 066, [2501.09280]

work page arXiv 2025
[43]

Collaviti, L

S. Collaviti, L. Sun, M. Galanis and M. Baryakhtar,Observational prospects of self-interacting scalar superradiance with next-generation gravitational-wave detectors,Class. Quant. Grav.42 (2025) 025006, [2407.04304]

work page arXiv 2025
[44]

Takahashi, H

T. Takahashi, H. Omiya and T. Tanaka,Self-interacting axion clouds around rotating black holes in binary systems,Phys. Rev. D110(2024) 104038, [2408.08349]

work page arXiv 2024
[45]

J. C. Aurrekoetxea, J. Marsden, K. Clough and P. G. Ferreira,Self-interacting scalar dark matter around binary black holes,Phys. Rev. D110(2024) 083011, [2409.01937]

work page arXiv 2024
[46]

A. L. Miller,Gravitational wave probes of particle dark matter: a review,2503.02607. – 20 –

work page arXiv
[47]

Xie and F

N. Xie and F. P. Huang,Self-interaction effects on the Kerr black hole superradiance and their observational implications,Phys. Rev. D112(2025) 055028, [2503.10347]

work page arXiv 2025
[48]

Superradiance in stars

V. Cardoso, R. Brito and J. L. Rosa,Superradiance in stars,Phys. Rev. D91(2015) 124026, [1505.05509]

work page internal anchor Pith review Pith/arXiv arXiv 2015
[49]

Superradiance in rotating stars and pulsar-timing constraints on dark photons

V. Cardoso, P. Pani and T.-T. Yu,Superradiance in rotating stars and pulsar-timing constraints on dark photons,Phys. Rev. D95(2017) 124056, [1704.06151]

work page internal anchor Pith review Pith/arXiv arXiv 2017
[50]

F. V. Day and J. I. McDonald,Axion superradiance in rotating neutron stars,JCAP10 (2019) 051, [1904.08341]

work page arXiv 2019
[51]

D. E. Kaplan, S. Rajendran and P. Riggins,Particle Probes with Superradiant Pulsars, 1908.10440

work page arXiv 1908
[52]

Chadha-Day, B

F. Chadha-Day, B. Garbrecht and J. McDonald,Superradiance in stars: non-equilibrium approach to damping of fields in stellar media,JCAP12(2022) 008, [2207.07662]

work page arXiv 2022
[53]

T. F. M. Spieksma and E. Cannizzaro,Axion dissipation in conductive media and neutron star superradiance,2503.19978

work page arXiv
[54]

Sirki¨ a, M

T. Sirki¨ a, M. Heikinheimo and K. Tuominen,Axion Superradiance in Dipole Magnetic Fields of Pulsars,2504.04209

work page arXiv
[55]

Black Hole Superradiance Signatures of Ultralight Vectors

M. Baryakhtar, R. Lasenby and M. Teo,Black Hole Superradiance Signatures of Ultralight Vectors,Phys. Rev. D96(2017) 035019, [1704.05081]

work page internal anchor Pith review Pith/arXiv arXiv 2017
[56]

Y. Chen, X. Xue, R. Brito and V. Cardoso,Photon Ring Astrometry for Superradiant Clouds, Phys. Rev. Lett.130(2023) 111401, [2211.03794]

work page arXiv 2023
[57]

B. L. Friman and O. V. Maxwell,Neutron Star Neutrino Emissivities,Astrophys. J.232 (1979) 541–557

work page 1979
[58]

Iwamoto,Axion Emission from Neutron Stars,Phys

N. Iwamoto,Axion Emission from Neutron Stars,Phys. Rev. Lett.53(1984) 1198–1201

work page 1984
[59]

R. P. Brinkmann and M. S. Turner,Numerical Rates for Nucleon-Nucleon Axion Bremsstrahlung,Phys. Rev. D38(1988) 2338

work page 1988
[60]

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) 2605–2608

work page 1991
[61]

Reduction of Weak Interaction Rates in Neutron Stars by Nucleon Spin Fluctuations: Degenerate Case

G. Raffelt and T. Strobel,Reduction of weak interaction rates in neutron stars by nucleon spin fluctuations: Degenerate case,Phys. Rev. D55(1997) 523–527, [astro-ph/9610193]

work page internal anchor Pith review Pith/arXiv arXiv 1997
[62]

P. S. Shternin, M. Baldo and P. Haensel,Transport coefficients of nuclear matter in neutron star cores,Phys. Rev. C88(2013) 065803, [1311.4278]

work page internal anchor Pith review Pith/arXiv arXiv 2013
[63]

Shternin and M

P. Shternin and M. Baldo,Transport coefficients of nucleon neutron star cores for various nuclear interactions within the Brueckner-Hartree-Fock approach,Phys. Rev. D102(2020) 063010, [2004.14909]

work page arXiv 2020
[64]

Baym and C

G. Baym and C. Pethick,Landau Fermi-Liquid Theory: Concepts and Applications. John Wiley & Sons, inc., New York, Chichester, Brisbane, Toronto, Singapore, 1991

work page 1991
[65]

Iwamoto,Nucleon-nucleon bremsstrahlung of axions and pseudoscalar particles from neutron star matter,Phys

N. Iwamoto,Nucleon-nucleon bremsstrahlung of axions and pseudoscalar particles from neutron star matter,Phys. Rev. D64(2001) 043002

work page 2001
[66]

Hoffmann,Paraphotons and Axions: Similarities in Stellar Emission and Detection,Phys

S. Hoffmann,Paraphotons and Axions: Similarities in Stellar Emission and Detection,Phys. Lett. B193(1987) 117–122

work page 1987
[67]

B. A. Dobrescu,Massless gauge bosons other than the photon,Phys. Rev. Lett.94(2005) 151802, [hep-ph/0411004]

work page internal anchor Pith review Pith/arXiv arXiv 2005
[68]

P. W. Graham and S. Rajendran,New Observables for Direct Detection of Axion Dark Matter,Phys. Rev. D88(2013) 035023, [1306.6088]. – 21 –

work page internal anchor Pith review Pith/arXiv arXiv 2013
[69]

Cosmic Axion Spin Precession Experiment (CASPEr)

D. Budker, P. W. Graham, M. Ledbetter, S. Rajendran and A. Sushkov,Proposal for a Cosmic Axion Spin Precession Experiment (CASPEr),Phys. Rev. X4(2014) 021030, [1306.6089]

work page internal anchor Pith review Pith/arXiv arXiv 2014
[70]

P. W. Graham, D. E. Kaplan, J. Mardon, S. Rajendran, W. A. Terrano, L. Trahms et al., Spin Precession Experiments for Light Axionic Dark Matter,Phys. Rev. D97(2018) 055006, [1709.07852]

work page internal anchor Pith review Pith/arXiv arXiv 2018
[71]

Jiang, H

M. Jiang, H. Su, A. Garcon, X. Peng and D. Budker,Search for axion-like dark matter with spin-based amplifiers,Nature Phys.17(2021) 1402–1407, [2102.01448]

work page arXiv 2021
[72]

Y. Chen, M. Jiang, J. Shu, X. Xue and Y. Zeng,Dissecting axion and dark photon with a network of vector sensors,Phys. Rev. Res.4(2022) 033080, [2111.06732]

work page arXiv 2022
[73]

Jiang, H

M. Jiang, H. Su, Y. Chen, M. Jiao, Y. Huang, Y. Wang et al.,Searches for exotic spin-dependent interactions with spin sensors,Rept. Prog. Phys.88(2025) 016401, [2412.03288]

work page arXiv 2025
[74]

C. S. Shin and S. Yun,Dark gauge boson production from neutron stars via nucleon-nucleon bremsstrahlung,JHEP02(2022) 133, [2110.03362]

work page arXiv 2022
[75]

L. B. Leinson,Axion mass limit from observations of the neutron star in Cassiopeia A,JCAP 08(2014) 031, [1405.6873]

work page internal anchor Pith review Pith/arXiv arXiv 2014
[76]

Limit on the Axion Decay Constant from the Cooling Neutron Star in Cassiopeia A

K. Hamaguchi, N. Nagata, K. Yanagi and J. Zheng,Limit on the Axion Decay Constant from the Cooling Neutron Star in Cassiopeia A,Phys. Rev. D98(2018) 103015, [1806.07151]

work page internal anchor Pith review Pith/arXiv arXiv 2018
[77]

Hamaguchi, N

K. Hamaguchi, N. Nagata and J. Zheng,Axion emission from proton Cooper pairs in neutron stars,JCAP06(2025) 038, [2502.18931]

work page arXiv 2025
[78]

D. K. Hong, C. S. Shin and S. Yun,Cooling of young neutron stars and dark gauge bosons, Phys. Rev. D103(2021) 123031, [2012.05427]

work page arXiv 2021
[79]

Pion mass effects on axion emission from neutron stars through NN bremsstrahlung processes

S. Stoica, B. Pastrav, J. E. Horvath and M. Allen,Pion mass effects on axion emission from neutron stars through nn bremsstrahlung processes,Nuclear Physics A828(2009) 439–449, [0906.3134]

work page internal anchor Pith review Pith/arXiv arXiv 2009
[80]

S. P. Harris,Transport in Neutron Star Mergers, Ph.D. thesis, Washington U., St. Louis, 2020.2005.09618. 10.7936/wrmz-1n98

work page doi:10.7936/wrmz-1n98 2020

Showing first 80 references.