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Boomerang mechanism explaining the excess radio background

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Pith's one-line read A two-stage 'boomerang' process lets relic neutrinos decay into the unexplained radio background while evading the magnetic-moment bound.

desk verdict Genuinely new two-stage mechanism for the ARCADE 2 excess, but the allowed parameter space relies on a lepton asymmetry that violates the paper's own BBN/CMB bound. read the letter →

arxiv 2509.03441 v3 pith:KVKV3KPI submitted 2025-09-03 hep-ph astro-ph.CO

Bhupal Dev , Pasquale Di Bari , Ivan Martinez-Soler , Rishav Roshan This is my paper · ORCID
classification hep-phastro-ph.CO
keywords excessradiobackgroundARCADE2relicneutrinoradiativedecaydarkleptonasymmetryresonantactive-sterileconversionphotonmagneticmoment
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

The paper argues that the unidentified 3–10 GHz radio background seen by the ARCADE 2 instrument can be produced by relic neutrinos that first switch identity in the hot early universe and then, much later, decay into photons. A direct radiative decay of relic neutrinos cannot explain the data, because the globular-cluster bound on the neutrino magnetic moment forces the required decay to be far too slow. The proposed 'boomerang mechanism' sidesteps this bound by splitting the process in two: a pre-existing lepton asymmetry induces a resonant conversion of a fraction of relic antineutrinos into dark neutrinos near T ≈ 0.1 keV–1 MeV, and those dark neutrinos later decay into a dark photon state carrying a small standard-photon component, generating the excess. The mechanism preserves the successful spectral fit to the six ARCADE 2 points while trading the heavily constrained active-neutrino magnetic moment for an effectively unconstrained dark-neutrino magnetic moment, and it predicts a lower bound on the effective active-neutrino magnetic moment of about 10^-16 Bohr magnetons, which future experiments could probe.

What carries the argument

The device carrying the argument is the two-stage decay chain. First, a pre-existing lepton asymmetry L_i shifts the early-universe neutrino potential so that only antineutrinos (for L_i > 0) hit a resonance below 1 MeV and convert into dark neutrinos; the converted fraction is set by the Landau-Zener factor f ≈ 1 − e^{−π γ_res/2}. Second, the dark neutrino ν_0 radiatively decays into a dark fermion ψ′ plus a photon-like state γ′ of energy ∆m′ = m_0 − m_ψ′, injecting the non-thermal photon spectrum of Eq. (1) with an extra factor ε(2/(1 − e^{−π γ_res/2}))^{-1}. The identity doing the work is µ_eff = √ε sin²θ_0 µ′_eff: the photon rate needed for the ARCADE 2 excess is provided by the unconstr

What would settle it

Point a spectrometer with enough sensitivity at 10–20 GHz—the TMS band—at the sky: the relic-decay explanation of the excess requires the radio temperature to follow the specific spectrum of Eq. (1), turning over and falling sharply above roughly 10 GHz (the photon cutoff set by ∆m_1 ≈ 4×10^-5 eV ≈ 9.7 GHz). A measured excess that continues as a power law well above 20 GHz, or a spectrum with a different turnover, would falsify the mechanism's source; likewise, a failure to detect any excess in 10–20 GHz consistent with the ARCADE 2 points would remove the phenomenon the mechanism aims to expl

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Extended reading notes

Core claim

The paper's central claim is that the ARCADE 2 excess can be explained by relic-neutrino decay if the decay is indirect: antineutrinos are first resonantly converted into quasi-degenerate dark neutrinos by a pre-existing lepton asymmetry, then decay into a dark fermion plus a mixed dark/standard photon state. The decay rate is set by a dark-neutrino effective magnetic moment µ′_eff, not directly constrained by stellar cooling, while the active neutrino's effective moment µ_eff = √ε sin²θ_0 µ′_eff is suppressed by the small mixing angle—evading the globular-cluster bound that kills direct decays. Matching the dark-neutrino lifetime to the earlier ARCADE 2 fit (∆m_1 ≈ 4×10^-5 eV, τ_1 ≈ 1.46×10

Load-bearing premise

The mechanism presupposes that a lepton asymmetry of magnitude roughly 10^-6 to 10^-2 with the correct sign already existed when the universe cooled below about 1 MeV; the paper treats this as an initial condition rather than generating it, and without it the resonant conversion of antineutrinos into dark neutrinos does not occur.

Editorial extensions

If this is right

  • A measurement in the 10–20 GHz band (the TMS window) is a direct discriminator: the predicted spectrum of Eq. (1) has a photon cutoff at the mass splitting ∆m_1 ≈ 4×10^-5 eV, i.e. near 10 GHz, so the excess should die out above the ARCADE 2 band rather than continue as a power law.
  • The mechanism requires a lepton asymmetry L_i in the 10^-6–10^-2 range; the paper notes that such an asymmetry is allowed by BBN and CMB bounds and could be responsible for other cosmological anomalies, and it leaves a modified 21 cm global signal as an independent probe.
  • A nonzero effective neutrino magnetic moment with µ_eff/µ_B ≳ 10^-16 is a robust prediction: future neutrino electromagnetic-property experiments can test this lower bound, and smaller L_i moves the bound upward, making the prediction easier to reach.
  • In the active-dark mixing plane (∆m², sin²2θ_0), the allowed region must survive existing solar, reactor, and long-baseline oscillation bounds; the paper identifies DARWIN and JUNO as upcoming searches that could discover the required pseudo-Dirac mixing or exclude it.
  • Because the conversion happens before neutrino decoupling, the mechanism implies non-standard relic-neutrino background properties that could in principle be measured, alongside potentially observable BBN/CMB effects of the large lepton asymmetry.

Reading between the lines

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

  • A testable extension the paper does not work out: the high-frequency side of the ERB spectrum measures ∆m_1 directly, so independent spectroscopy above 10 GHz could determine the dark-neutrino mass splitting without using the ARCADE 2 fit.
  • If the initial asymmetry is generated by the active-dark mixing itself (the dynamic option mentioned in the paper), the sign of L_i—and hence whether neutrinos or antineutrinos are converted—is fixed by the first resonance; tracking this numerically during BBN would turn the mechanism into a predictive, not parametric, scenario.
  • The visible-to-dark-to-visible template could in principle be reused for other smooth diffuse backgrounds (21 cm anomalies, X-ray/IR excesses) by choosing different mass splittings and lifetimes, with the same evasion of stellar-cooling bounds.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

1 major / 5 minor

Summary. The paper proposes a two-stage 'boomerang' mechanism to explain the ARCADE 2 excess radio background. A pre-existing effective muon lepton asymmetry Li causes resonant conversion of relic antineutrinos into quasi-degenerate dark neutrinos at temperatures ~0.1 keV–1 MeV. These dark neutrinos subsequently decay into a superposition of dark and standard photons, with a lifetime fixed by Eq. (19) to reproduce the ERB fit from the authors' earlier paper [7]. The mechanism trades the active neutrino transition magnetic moment for a dark-sector magnetic moment, thereby evading the globular-cluster bound (5), and yields a lower bound mu_eff/mu_B >~ 10^-16. The paper determines an allowed region in the (Delta m^2, sin^2 2theta_0) plane and compares it with sterile-neutrino oscillation constraints.

Significance. The central idea—moving the decay magnetic moment into the dark sector and connecting the two sectors through an asymmetry-induced resonance—is original and potentially testable. The paper is clearly written, builds on a quantitative previous fit to ARCADE 2, and includes a useful comparison with oscillation bounds. It also candidly discusses model-building caveats (millicharge, stellar cooling, UV completion). The derived lower bound on the active effective magnetic moment is a genuine consequence of the mechanism and could be probed by future experiments. However, the main concern identified below—the self-consistency of the lepton asymmetry evolution—is load-bearing for the allowed region and must be addressed before the central claim can be accepted.

major comments (1)
  1. [Active-to-dark neutrino conversions; Eqs. (15)-(19)] The paper imposes the cosmological bound Li <~ 10^-2 (Ref. [27]) only on the initial asymmetry, but Eq. (17) uses <L> ~ Lf/2 ~ 0.2, implying Lf ~ 0.4 after antineutrino conversion. Since conversion removes antineutrinos from the active sector, the active asymmetry grows by O(n_nu/n_gamma) ~ O(0.1-1); a self-consistent adiabatic sweep thus produces Lf ~ 0.4 at T_res < 1 MeV, violating the BBN/CMB bound |L| <~ 0.01 cited in the same paper. If L is instead kept <~ 0.01, gamma_res in Eq. (17) is overestimated by roughly (0.2/0.01)^{3/4} ~ 9.5, shrinking or eliminating the allowed region in Fig. 3 and the lower bound mu_eff >~ 10^-16. The paper does not address this growth or verify the final asymmetry. This is load-bearing for the central claim and needs a self-consistent treatment.
minor comments (5)
  1. [Dark neutrino decays / Eq. (19)] Eq. (19) writes the reduction factor as (1 - e^{-gamma_res})/2, but the conversion probability in Eq. (15) is 1 - e^{-pi/2 gamma_res}; the text immediately before Eq. (19) uses the correct exponent. Please correct Eq. (19) and check the numerical impact on the derived mu_eff bound.
  2. [Constraints and allowed region] The sentence 'we have to impose that the dark neutrino lifetime is given by the lifetime determined in [7]' is better phrased as 'we fix the lifetime to the value required to reproduce the ARCADE 2 fit.' The current wording makes the fit condition sound like an external input.
  3. [Conclusions] The lower bound mu_eff/mu_B >~ 10^-16 is a consequence of requiring the mechanism to fit the ARCADE 2 excess; it is not an independent prediction. The abstract and conclusions should state this more explicitly.
  4. [Final remarks (v)] The statement 'they would disappear for a lower bound epsilon ~ 2 x 10^-4' should read 'for a lower value epsilon ~ 2 x 10^-4'; also, give the reference or derivation for this threshold.
  5. [General] There is a typo 'branching ration' in the dark neutrino decay section; also the phrase 'divided by a factor 2/(1 - e^{-pi/2 gamma_res})' could be simplified to 'multiplied by epsilon (1 - e^{-pi/2 gamma_res})/2'.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the ARCADE-2 fit is imported from prior work but is external data fitting, and the derived magnetic-moment bound is a genuine consistency constraint rather than a disguised fit.

full rationale

The paper's central claim is that the boomerang mechanism can realize the radiative relic neutrino decay solution to the ARCADE-2 excess while evading the globular-cluster bound. The derivation chain is: (i) import the previous fit of the ARCADE-2 data from Ref. [7], which fixes the required combination Δm^(3/2) τ for direct neutrino decays; (ii) construct an active–dark neutrino conversion plus dark neutrino decay scenario; (iii) impose Eq. (19) so that the dark neutrino lifetime is set to reproduce the same ARCADE-2 effective temperature; (iv) translate this lifetime into a dark neutrino magnetic moment via Eq. (18) and then into an active effective magnetic moment through μ_eff = √ε sin²θ0 μ'_eff. Step (iii) is a deliberate fitting condition, not a hidden prediction: the paper does not claim to predict the ARCADE-2 spectrum from first principles, but rather to show that a parameter region exists satisfying all constraints. The resulting lower bound μ_eff/μ_B ≳ 10^-16 is a testable consequence of the fit, not a statistically forced prediction of the same data. The self-citations to Ref. [7] and Ref. [20] are load-bearing but rest on independent published analyses: Ref. [7] is a fit to public ARCADE-2 data, and Ref. [20] provides numerical results for the Landau-Zener approximation and asymmetry evolution. No uniqueness theorem or ansatz is smuggled in. A physical-consistency concern (not circularity) is raised by the use of ⟨L⟩ ≃ 0.2 in Eq. (17) while bounding only the initial asymmetry L_i ≲ 10^-2; this may be a correctness issue, but it does not amount to the derivation being equivalent to its inputs. The paper also checks the allowed region against external oscillation bounds in Fig. 4, making it self-contained against independent benchmarks. Therefore no significant circularity is present.

Assumptions & free parameters 6 free parameters · 5 assumptions · 3 invented entities

The mechanism rests on a pre-existing lepton asymmetry, a dark neutrino/photon/fermion sector with hand-set mass splittings, and a photon detection probability ε. The only numerical inputs from external fits are the ARCADE 2 data points and the lifetime/amplitude fitted in the authors' prior paper [7], which are inherited rather than derived here.

free parameters (6)
  • L_i (initial effective muonic lepton asymmetry) = assumed in range L* < |L_i| ≤ 10^-2
    Required to make the resonant conversion happen at T_res < 1 MeV; not derived in the model.
  • ε (probability the dark photon state is detected as ordinary photon) = set to 1 (conservative); lower limit ~2×10^-4
    Parameterizes the dark photon mixing; not derived from kinetic mixing.
  • m_γ' (dark photon mass) = < 10^-15 eV
    Chosen to evade COBE/FIRAS constraints; not derived.
  • µ'_eff (dark neutrino effective magnetic moment) = ~1.6×10^-5 µB from τ_ARCADE
    Set by Eq. (19) to match the fitted lifetime; effectively a derived fit parameter.
  • y_res and ⟨L⟩ (monochromatic approximation parameters) = y_res = 3.15, ⟨L⟩ = 0.2
    Taken from Ref. [20]; adopted for the Landau-Zener conversion fraction.
  • ∆m' (dark mass splitting) = ~4×10^-5 eV
    Implicitly identified with the active-neutrino mass splitting ∆m1 from the ARCADE fit.
assumptions (5)
  • standard math MSW resonant conversion between active and dark neutrinos with effective potential from finite temperature and lepton asymmetry
    Used in Eqs. (8)-(13); standard extension of neutrino oscillations to medium.
  • domain assumption Landau-Zener formula (Eqs. 15-16) describes the conversion probability for non-adiabatic level crossing
    Adopted from ref [20]; relies on linear level crossing and monochromatic approximation.
  • ad hoc to paper A pre-existing lepton asymmetry L_i exists with appropriate magnitude and sign
    Assumed after Eq. (12); not generated in the model (though final remarks mention dynamical generation as an option).
  • domain assumption Dark neutrino decays to dark fermion plus dark photon with mass splitting ∆m' comparable to the active neutrino splitting
    Needed for the decay product to reproduce the observed ERB spectrum; no full model given.
  • domain assumption The dark photon has mass below 10^-15 eV and mixes with the ordinary photon with probability ε
    Introduced to evade COBE/FIRAS constraints on photon-dark photon mixing.
invented entities (3)
  • Dark neutrino ν0 (light sterile state)
    purpose: Intermediate state for the boomerang conversion and decay
    Postulated to be quasi-degenerate with the lightest active neutrino and to mix only with muon neutrino; no independent detection.
  • Dark fermion ψ'
    purpose: Final state of dark neutrino decay
    Assumed quasi-degenerate with ν0; no independent evidence.
  • Dark photon γ'
    purpose: Carries the energy later observed as the radio background; mixes with photon with probability ε
    Mass assumed below 10^-15 eV to avoid CMB spectral distortion bounds; not detected.

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Cite this review

Pith. "Pith review of Boomerang mechanism explaining the excess radio background." pith.science (2026). https://pith.science/paper/KVKV3KPI

@misc{pith2026250903441,
  author       = {Pith},
  title        = {Pith review of: Boomerang mechanism explaining the excess radio background},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/KVKV3KPI}},
  note         = {Machine review of arXiv:2509.03441}
}
abstract

We propose a boomerang mechanism for the explanation of the excess radio background detected by ARCADE 2. In an early stage of the Universe, at a temperature $T$ in the range $\sim 0.1\,{\rm keV}$--$1\,{\rm MeV}$, a fraction of relic neutrinos is resonantly converted into dark neutrinos by mixing induced by a pre-existing lepton asymmetry. Dark neutrinos decay much later into a dark-standard photon state and a dark fermion, with a lifetime longer than the age of the Universe, as required by a solution to the excess radio background. This scenario circumvents the upper bound on the neutrino magnetic moment but still implies a testable lower bound.

Figures

Figures reproduced from arXiv: 2509.03441 by the authors.

Figure 1
Figure 1. FIG. 1. Best fit curve for [PITH_FULL_IMAGE:figures/full_fig_p001_1.png] view at source ↗
Figure 2
Figure 2. FIG. 2. Allowed region shaded with different shades cor [PITH_FULL_IMAGE:figures/full_fig_p002_2.png] view at source ↗
Figure 3
Figure 3. FIG. 3. Left panel: Constraints (shaded) and allowed region (white) in the plane of ∆ [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figures from the paper (1 more)
Figure 4
Figure 4. Figure 4: FIG. 4. Region allowed by the boomerang mechanism at [PITH_FULL_IMAGE:figures/full_fig_p006_4.png]

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Reference graph

Works this paper leans on

72 extracted references · 17 canonical work pages · cited by 2 Pith papers

  1. [7]

    P. S. B. Dev, P. Di Bari, I. Mart ´ ınez-Soler, and R. Roshan, Relic neutrino decay solution to the excess radio background, JCAP 04, 046, arXiv:2312.03082 [hep- ph]

    arXiv

  2. [27]

    A. D. Dolgov, S. H. Hansen, S. Pastor, S. T. Petcov, G. G. Raffelt, and D. V. Semikoz, Cosmological bounds on neutrino degeneracy improved by flavor oscillations, Nucl. Phys. B 632, 363 (2002), arXiv:hep-ph/0201287

    arXiv 2002

  3. [1]

    D. J. Fixsen et al., ARCADE 2 Measurement of the Extra-Galactic Sky Temperature at 3-90 GHz, Astro- phys. J. 734, 5 (2011), arXiv:0901.0555 [astro-ph.CO]

    arXiv 2011

  4. [2]

    Singal et al., The Radio Synchrotron Background: Conference Summary and Report, Publ

    J. Singal et al., The Radio Synchrotron Background: Conference Summary and Report, Publ. Astron. Soc. Pac. 130, 036001 (2018), arXiv:1711.09979 [astro- ph.HE]

    arXiv 2018

  5. [3]

    G. P. Holder, The unusual smoothness of the extragalac- tic unresolved radio background, Astrophys. J. 780, 112 (2014), arXiv:1207.0856 [astro-ph.CO]

    arXiv 2014

  6. [4]

    J. A. Rubi˜ no Mart ´ ınet al., The Tenerife Microwave Spectrometer (TMS) experiment: studying the absolute spectrum of the sky emission in the 10-20GHz range, in Millimeter, Submillimeter, and Far-Infrared Detec- tors and Instrumentation for Astronomy X, Society of Photo-Optical Instrumentation Engineers (SPIE) Con- 10−13 10−11 10−9 10−7 10−5 10−3 10−1 s...

    work page 2020

  7. [5]

    The optical system of the Tenerife Microwave Spectrometer: a window for observing the 10-20 GHz sky spectra

    P. Alonso-Arias, P. A. Fuerte-Rodr ´ ıguez, R. J. Hoyland, and J. A. Rubi˜ no-Mart ´ ın, The optical system of the Tenerife Microwave Spectrometer: a window for observ- ing the 10–20 GHz sky spectra, JINST 16 (12), P12037, arXiv:2111.15364 [astro-ph.IM]

    work page Pith review arXiv

  8. [6]

    Chianese, P

    M. Chianese, P. Di Bari, K. Farrag, and R. Samanta, Probing relic neutrino radiative decays with 21 cm cos- mology, Phys. Lett. B 790, 64 (2019), arXiv:1805.11717 [hep-ph]

    arXiv 2019

Show all 72 references
  1. [8]

    D. J. Fixsen, The Temperature of the Cosmic Mi- crowave Background, Astrophys. J. 707, 916 (2009), arXiv:0911.1955 [astro-ph.CO]

    2009 arXiv

  2. [9]

    Dowell and G

    J. Dowell and G. B. Taylor, The Radio Background Below 100 MHz, Astrophys. J. Lett. 858, L9 (2018), arXiv:1804.08581 [astro-ph.CO]

    2018 arXiv

  3. [10]

    Xing and S

    Z.-z. Xing and S. Zhou, Neutrinos in particle physics, astronomy and cosmology(2011)

    2011

  4. [11]

    Giunti and A

    C. Giunti and A. Studenikin, Neutrino electromagnetic interactions: a window to new physics, Rev. Mod. Phys. 87, 531 (2015), arXiv:1403.6344 [hep-ph]

    2015 arXiv

  5. [12]

    G. G. Raffelt, New bound on neutrino dipole moments from globular cluster stars, Phys. Rev. Lett. 64, 2856 (1990)

    1990

  6. [13]

    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. D 102, 083007 (2020), arXiv:2007.03694 [astro- ph.SR]

    2020 arXiv

  7. [14]

    A. G. Beda, V. B. Brudanin, V. G. Egorov, D. V. 7 Medvedev, V. S. Pogosov, M. V. Shirchenko, and A. S. Starostin, Upper limit on the neutrino magnetic moment from three years of data from the GEMMA spectrometer, (2010), arXiv:1005.2736 [hep-ex]

    2010 arXiv

  8. [15]

    A. G. Beda, V. B. Brudanin, V. G. Egorov, D. V. Medvedev, V. S. Pogosov, M. V. Shirchenko, and A. S. Starostin, The results of search for the neutrino mag- netic moment in GEMMA experiment, Adv. High Energy Phys. 2012, 350150 (2012)

    2012

  9. [16]

    The net result is that neutrinos are converted into photons

    The name ‘boomerang’ mechanism is justified by the fact that the visible sector first throws sterile neutrinos into the dark sector via mixing, and then these, decaying, throw back photons into the visible sector. The net result is that neutrinos are converted into photons. Tr...

  10. [17]

    We adopt a different sign convention for ∆m2 than in [20, 21]

  11. [18]

    N¨ otzold and G

    D. N¨ otzold and G. Raffelt, Neutrino dispersion at finite temperature and density, Nucl. Phys. B 307, 924 (1988)

    1988

  12. [19]

    R. Foot, M. J. Thomson, and R. R. Volkas, Large neu- trino asymmetries from neutrino oscillations, Phys. Rev. D 53, R5349 (1996), arXiv:hep-ph/9509327

    1996 arXiv

  13. [20]

    Di Bari and R

    P. Di Bari and R. Foot, Active sterile neutrino oscillations in the early universe: Asymmetry generation at low|δm2| and the Landau-Zener approximation, Phys. Rev. D 65, 045003 (2002), arXiv:hep-ph/0103192

    2002 arXiv

  14. [21]

    Enqvist, K

    K. Enqvist, K. Kainulainen, and J. Maalampi, Refraction and Oscillations of Neutrinos in the Early Universe, Nucl. Phys. B 349, 754 (1991)

    1991

  15. [22]

    Mirizzi, J

    A. Mirizzi, J. Redondo, and G. Sigl, Microwave Back- ground Constraints on Mixing of Photons with Hidden Photons, JCAP 03, 026, arXiv:0901.0014 [hep-ph]

    arXiv

  16. [23]

    Caputo, H

    A. Caputo, H. Liu, S. Mishra-Sharma, and J. T. Ru- derman, Dark Photon Oscillations in Our Inhomoge- neous Universe, Phys. Rev. Lett. 125, 221303 (2020), arXiv:2002.05165 [astro-ph.CO]

    2020 arXiv

  17. [24]

    A. A. Garcia, K. Bondarenko, S. Ploeckinger, J. Pradler, and A. Sokolenko, Effective photon mass and (dark) pho- ton conversion in the inhomogeneous Universe, JCAP10, 011, arXiv:2003.10465 [astro-ph.CO]

    2003 arXiv

  18. [25]

    Arsenadze, A

    G. Arsenadze, A. Caputo, X. Gan, H. Liu, and J. T. Ru- derman, Shaping dark photon spectral distortions, JHEP 03, 018, arXiv:2409.12940 [astro-ph.CO]

    arXiv

  19. [26]

    Here we do not assume the dark photon to be dark matter in which case the bounds on mγ′ would be more strin- gent [71]. Moreover, we do not consider the Juno con- straint on mγ′ that extends down tomγ′ ∼ 10−18 eV [72], as we lack a detailed understanding of the Jovian mag- net...

  20. [28]

    Giunti, K

    C. Giunti, K. Kouzakov, Y.-F. Li, and A. Studenikin, Neutrino Electromagnetic Properties 10.1146/annurev- nucl-102122-023242 (2024), arXiv:2411.03122 [hep-ph]

    2024 arXiv

  21. [29]

    Burns, T

    A.-K. Burns, T. M. P. Tait, and M. Valli, Indications for a Nonzero Lepton Asymmetry from Extremely Metal- Poor Galaxies, Phys. Rev. Lett. 130, 131001 (2023), arXiv:2206.00693 [hep-ph]

    2023 arXiv

  22. [30]

    Fukugita and T

    M. Fukugita and T. Yanagida, Baryogenesis Without Grand Unification, Phys. Lett. B 174, 45 (1986)

    1986

  23. [31]

    DeRocco, P

    W. DeRocco, P. W. Graham, and S. Rajendran, Ex- ploring the robustness of stellar cooling constraints on light particles, Phys. Rev. D 102, 075015 (2020), arXiv:2006.15112 [hep-ph]

    2020 arXiv

  24. [32]

    R. N. Mohapatra and S. Nasri, Reconciling the CAST and PVLAS results, Phys. Rev. Lett. 98, 050402 (2007), arXiv:hep-ph/0610068

    2007 arXiv

  25. [33]

    Di Bari and M

    P. Di Bari and M. H. Rahat, Split Majoron model con- fronts the NANOGrav signal and cosmological tensions, Phys. Rev. D 110, 055019 (2024), arXiv:2307.03184 [hep- ph]

    2024 arXiv

  26. [34]

    K. S. Babu, X.-G. He, M. Su, and A. Thapa, Naturally light Dirac and pseudo-Dirac neutrinos from left-right symmetry, JHEP 08, 140, arXiv:2205.09127 [hep-ph]

    arXiv

  27. [35]

    Carloni, I

    K. Carloni, I. Mart ´ ınez-Soler, C. A. Arguelles, K. S. Babu, and P. S. B. Dev, Probing pseudo-Dirac neutri- nos with astrophysical sources at IceCube, Phys. Rev. D 109, L051702 (2024), arXiv:2212.00737 [astro-ph.HE]

    2024 arXiv

  28. [36]

    Kersten and A

    J. Kersten and A. Y. Smirnov, Right-Handed Neutri- nos at CERN LHC and the Mechanism of Neutrino Mass Generation, Phys. Rev. D 76, 073005 (2007), arXiv:0705.3221 [hep-ph]

    2007 arXiv

  29. [37]

    Aguilar et al

    A. Aguilar et al. (LSND), Evidence for neutrino oscilla- tions from the observation of ¯νe appearance in a ¯νµ beam, Phys. Rev. D 64, 112007 (2001), arXiv:hep-ex/0104049

    2001 arXiv

  30. [38]

    A. A. Aguilar-Arevalo et al. (MiniBooNE), Updated MiniBooNE neutrino oscillation results with increased data and new background studies, Phys. Rev. D 103, 052002 (2021), arXiv:2006.16883 [hep-ex]

    2021 arXiv

  31. [39]

    V. V. Barinov et al., Results from the Baksan Exper- iment on Sterile Transitions (BEST), Phys. Rev. Lett. 128, 232501 (2022), arXiv:2109.11482 [nucl-ex]

    2022 arXiv

  32. [40]

    Abbasi et al

    R. Abbasi et al. ((IceCube Collaboration) ∥, IceCube), Search for an eV-Scale Sterile Neutrino Using Improved High-Energy νµ Event Reconstruction in IceCube, Phys. Rev. Lett. 133, 201804 (2024), arXiv:2405.08070 [hep- ex]

    2024

  33. [41]

    Dentler, ´A

    M. Dentler, ´A. Hern´ andez-Cabezudo, J. Kopp, P. A. N. Machado, M. Maltoni, I. Martinez-Soler, and T. Schwetz, Updated Global Analysis of Neutrino Oscillations in the Presence of eV-Scale Sterile Neutrinos, JHEP 08, 010, arXiv:1803.10661 [hep-ph]

    arXiv

  34. [42]

    J. M. Hardin, I. Martinez-Soler, A. Diaz, M. Jin, N. W. Kamp, C. A. Arg¨ uelles, J. M. Conrad, and M. H. Shae- vitz, New Clues about light sterile neutrinos: preference for models with damping effects in global fits, JHEP 09, 058, arXiv:2211.02610 [hep-ph]

    arXiv

  35. [43]

    Wolfenstein, Different Varieties of Massive Dirac Neu- trinos, Nucl

    L. Wolfenstein, Different Varieties of Massive Dirac Neu- trinos, Nucl. Phys. B 186, 147 (1981)

    1981

  36. [44]

    S. T. Petcov, On Pseudodirac Neutrinos, Neutrino Oscil- lations and Neutrinoless Double beta Decay, Phys. Lett. B 110, 245 (1982)

    1982

  37. [45]

    S. M. Bilenky and B. Pontecorvo, Neutrino Oscillations With Large Oscillation Length in Spite of Large (Ma- jorana) Neutrino Masses?, Sov. J. Nucl. Phys. 38, 248 (1983)

    1983

  38. [46]

    Kobayashi and C

    M. Kobayashi and C. S. Lim, Pseudo Dirac scenario for neutrino oscillations, Phys. Rev. D 64, 013003 (2001), arXiv:hep-ph/0012266

    2001 arXiv

  39. [47]

    Anamiati, R

    G. Anamiati, R. M. Fonseca, and M. Hirsch, Quasi Dirac neutrino oscillations, Phys. Rev. D 97, 095008 (2018), arXiv:1710.06249 [hep-ph]. 8

    2018 arXiv

  40. [48]

    de Gouvea, W.-C

    A. de Gouvea, W.-C. Huang, and J. Jenkins, Pseudo- Dirac Neutrinos in the New Standard Model, Phys. Rev. D 80, 073007 (2009), arXiv:0906.1611 [hep-ph]

    2009 arXiv

  41. [49]

    Vissani and A

    F. Vissani and A. Boeltzig, Supernova Neutrinos: Risks and Opportunities, PoS NEUTEL2015, 008 (2015)

    2015

  42. [50]

    I. M. Shoemaker and K. Murase, Probing BSM Neutrino Physics with Flavor and Spectral Distortions: Prospects for Future High-Energy Neutrino Telescopes, Phys. Rev. D 93, 085004 (2016), arXiv:1512.07228 [astro-ph.HE]

    2016 arXiv

  43. [51]

    Brdar and R

    V. Brdar and R. S. L. Hansen, IceCube Flavor Ra- tios with Identified Astrophysical Sources: Towards Improving New Physics Testability, JCAP 02, 023, arXiv:1812.05541 [hep-ph]

    arXiv

  44. [52]

    De Gouvˆ ea, I

    A. De Gouvˆ ea, I. Martinez-Soler, Y. F. Perez-Gonzalez, and M. Sen, Fundamental physics with the diffuse super- nova background neutrinos, Phys. Rev. D 102, 123012 (2020), arXiv:2007.13748 [hep-ph]

    2020 arXiv

  45. [53]

    Rink and M

    T. Rink and M. Sen, Constraints on pseudo-Dirac neutri- nos using high-energy neutrinos from NGC 1068, Phys. Lett. B 851, 138558 (2024), arXiv:2211.16520 [hep-ph]

    2024 arXiv

  46. [54]

    Ansarifard and Y

    S. Ansarifard and Y. Farzan, Revisiting pseudo-Dirac neutrino scenario after recent solar neutrino data, Phys. Rev. D 107, 075029 (2023), arXiv:2211.09105 [hep-ph]

    2023 arXiv

  47. [55]

    Z. Chen, J. Liao, J. Ling, and B. Yue, Constraining super- light sterile neutrinos at Borexino and KamLAND, JHEP 09, 004, arXiv:2205.07574 [hep-ph]

    arXiv

  48. [56]

    F. P. An et al. (Daya Bay), Search for a Sub-eV Sterile Neutrino using Daya Bay’s Full Dataset, Phys. Rev. Lett. 133, 051801 (2024), arXiv:2404.01687 [hep-ex]

    2024

  49. [57]

    Adamson et al.(MINOS+), Search for sterile neutrinos in MINOS and MINOS+ using a two-detector fit, Phys

    P. Adamson et al.(MINOS+), Search for sterile neutrinos in MINOS and MINOS+ using a two-detector fit, Phys. Rev. Lett. 122, 091803 (2019), arXiv:1710.06488 [hep- ex]

    2019 arXiv

  50. [58]

    M. A. Acero et al. (NOvA), Dual-Baseline Search for Active-to-Sterile Neutrino Oscillations in NOvA, Phys. Rev. Lett. 134, 081804 (2025), arXiv:2409.04553 [hep- ex]

    2025 arXiv

  51. [59]

    J. F. Beacom, N. F. Bell, D. Hooper, J. G. Learned, S. Pakvasa, and T. J. Weiler, PseudoDirac neutrinos: A Challenge for neutrino telescopes, Phys. Rev. Lett. 92, 011101 (2004), arXiv:hep-ph/0307151

    2004 arXiv

  52. [60]

    Martinez-Soler, Y

    I. Martinez-Soler, Y. F. Perez-Gonzalez, and M. Sen, Signs of pseudo-Dirac neutrinos in SN1987A data, Phys. Rev. D 105, 095019 (2022), arXiv:2105.12736 [hep-ph]

    2022 arXiv

  53. [61]

    de Gouvˆ ea, E

    A. de Gouvˆ ea, E. McGinness, I. Martinez-Soler, and Y. F. Perez-Gonzalez, pp solar neutrinos at DAR WIN, Phys. Rev. D 106, 096017 (2022), arXiv:2111.02421 [hep-ph]

    2022 arXiv

  54. [62]

    C. S. Fong and Y. Porto, Constraining pseudo- Diracness with astrophysical neutrino flavors, (2024), arXiv:2406.15566 [hep-ph]

    2024

  55. [63]

    P. S. B. Dev, P. A. N. Machado, and I. Martinez-Soler, Pseudo-Dirac neutrinos and relic neutrino matter effect on the high-energy neutrino flavor composition, Phys. Lett. B 862, 139306 (2025), arXiv:2406.18507 [hep-ph]

    2025 arXiv

  56. [64]

    Carloni, Y

    K. Carloni, Y. Porto, C. A. Arg¨ uelles, P. S. B. Dev, and S. Jana, Signatures of quasi-Dirac neutrinos in dif- fuse high-energy astrophysical neutrino data, (2025), arXiv:2503.19960 [hep-ph]

    2025

  57. [65]

    Franklin, Y

    J. Franklin, Y. F. Perez-Gonzalez, and J. Turner, JUNO as a probe of the pseudo-Dirac nature using solar neutri- nos, Phys. Rev. D 108, 035010 (2023), arXiv:2304.05418 [hep-ph]

    2023 arXiv

  58. [66]

    Hampel et al

    W. Hampel et al. (GALLEX), GALLEX solar neutrino observations: Results for GALLEX IV, Phys. Lett. B 447, 127 (1999)

    1999

  59. [67]

    B. T. Cleveland, T. Daily, R. Davis, Jr., J. R. Distel, K. Lande, C. K. Lee, P. S. Wildenhain, and J. Ullman, Measurement of the solar electron neutrino flux with the Homestake chlorine detector, Astrophys. J. 496, 505 (1998)

    1998

  60. [68]

    Q. R. Ahmad et al. (SNO), Direct evidence for neutrino flavor transformation from neutral current interactions in the Sudbury Neutrino Observatory, Phys. Rev. Lett. 89, 011301 (2002), arXiv:nucl-ex/0204008

    2002 arXiv

  61. [69]

    Fukuda et al

    S. Fukuda et al. (Super-Kamiokande), Solar B-8 and hep neutrino measurements from 1258 days of Super- Kamiokande data, Phys. Rev. Lett. 86, 5651 (2001), arXiv:hep-ex/0103032

    2001 arXiv

  62. [70]

    Aristizabal Sierra and C

    D. Aristizabal Sierra and C. S. Fong, The EDGES signal: An imprint from the mirror world?, Phys. Lett. B 784, 130 (2018), arXiv:1805.02685 [hep-ph]

    2018 arXiv

  63. [71]

    Caputo, A

    A. Caputo, A. J. Millar, C. A. J. O’Hare, and E. Vitagliano, Dark photon limits: A handbook, Phys. Rev. D 104, 095029 (2021), arXiv:2105.04565 [hep-ph]

    2021 arXiv

  64. [72]

    S. Yan, L. Li, and J. Fan, Constraints on photon mass and dark photon from the Jovian magnetic field, JHEP 06, 028, arXiv:2312.06746 [hep-ph]

    arXiv

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