arxiv: 2605.02547 · v1 · submitted 2026-05-04 · ✦ hep-ph

Recognition: 3 theorem links

· Lean Theorem

How neutrinos could help solving cosmological anomalies and tensions

Pasquale Di Bari

Authors on Pith no claims yet

Pith reviewed 2026-05-08 18:33 UTC · model grok-4.3

classification ✦ hep-ph

keywords neutrino decayscosmological tensionsneutrino massradio backgrounddark sectormagnetic moment21 cm signal

0 comments

The pith

Invisible decays of relic neutrinos can reconcile cosmological mass limits with lab measurements, and a boomerang dark-sector process can explain the radio background excess via radiative decays.

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

The paper proposes that neutrinos offer solutions to two cosmological issues. First, invisible decays of the heaviest relic neutrinos would lower their contribution to the universe's energy density, aligning the mass bound from cosmology with the higher values from oscillation experiments. Second, radiative decays could produce the excess radio background, but to avoid bounds on the neutrino magnetic moment, a boomerang mechanism is introduced: neutrinos move to a dark sector at around 100 seconds after the Big Bang and photons return much later. This predicts an effective magnetic moment detectable soon and a possible imprint on the 21 cm signal. These ideas matter because they turn puzzling observations into potential evidence for new physics testable in laboratories and with radio telescopes.

Core claim

The author claims that invisible decays of the heaviest relic neutrinos provide a way to solve the neutrino mass tension between cosmological observations and neutrino oscillation experiments, while a recently proposed boomerang mechanism allows radiative decays of relic neutrinos to explain the excess radio background mystery by transferring neutrinos to the dark sector at t ~ 100 s and returning photons at present times, predicting an effective neutrino magnetic moment within reach of next experiments and some contribution to the 21 cm signal.

What carries the argument

The boomerang mechanism, a two-stage transfer where the visible sector sends dark neutrinos into the dark sector early and the dark sector returns photons to the visible sector late, enabling radiative decays without violating magnetic moment constraints.

If this is right

The neutrino mass tension between cosmology and oscillation experiments is resolved if the heaviest neutrinos decay invisibly.
The excess radio background arises from photons returned by the dark sector at late times.
The predicted effective neutrino magnetic moment falls within the sensitivity of upcoming laboratory experiments.
The 21 cm cosmological signal receives an additional contribution from the decay process.

Where Pith is reading between the lines

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

Laboratory bounds on the neutrino magnetic moment could directly test the dark sector coupling proposed here.
If the mechanism holds, similar hidden-sector transfers might address other early-universe anomalies without new visible particles.
Radio surveys targeting late-time photon injection could provide independent evidence alongside magnetic moment searches.

Load-bearing premise

The dark sector must couple to neutrinos in a way that allows early transfer without affecting standard cosmology and later photon return while producing the required magnetic moment, details of which are not specified.

What would settle it

A measurement of the effective neutrino magnetic moment by next-generation experiments that falls outside the range allowed by the boomerang mechanism, or the absence of the expected 21 cm signal contribution, would rule out this explanation for the radio background.

Figures

Figures reproduced from arXiv: 2605.02547 by Pasquale Di Bari.

**Figure 1.** Figure 1: Map of new physics hints, evidences, opportunities. The background map is the famous Cantino planisphere (1502). 1. Introduction Extensions of the standard model are very strenuously and effectively tested by colliders that are so far placing more and more stringent constraints, pushing the border where new physics could lie at higher energy scales and smaller couplings. However, new physics could lie in a… view at source ↗

**Figure 2.** Figure 2: Plot of 𝑇ERB(𝜈) measured by ARCADE 2 for six values of 𝜈 as indicated. The grey band is a power law fit, the dashed vertical line is the low frequency threshold of the Tenerife Microwave Spectrometer (courtesy of Rishav Roshan). 3. The excess radio background mystery The FIRAS instrument of COBE has measured the spectrum of the cosmic microwave background (CMB) in the frequency range (60 – 600) GHz, corre… view at source ↗

**Figure 3.** Figure 3: Best fit curves for 𝑇ERB obtained with Eq. (18). The thick solid orange curve corresponds to a solution very close to the best global fit (Δ𝑚1 = 4.0 × 10−5 eV and 𝜏1 = 1.46 × 1021 s). The ARCADE 2 data points are taken from Ref. [14], while the power-law fit 𝛽 = −2.58 ± 0.05 (dotted line with grey shade) is from [20]. The figure is taken from [1]. For 𝑧 = 0, one recovers Eq. (9). The expansion rate at the … view at source ↗

**Figure 4.** Figure 4: Lower bounds on the radiative neutrino decay lifetime derived from Eq. (20) using the upper bounds in Eq. (21) on the effective neutrino magnetic moment. The figure is taken from [1] view at source ↗

**Figure 5.** Figure 5: Sketch of the boomerang mechanism proposed in [1]. 8 view at source ↗

**Figure 6.** Figure 6: Left panel: Constraints (shaded) and allowed region (white) in the plane of Δ𝑚 2 versus sin2 2𝜃0. The horizontal dashed lines give an upper bound on Δ𝑚 2 from 𝑇 res 𝜈 < 1 MeV for the indicated values of the initial lepton asymmetry 𝐿i . Right panel: Constraints (shaded) and allowed region (white) in the plane of 𝜇eff versus 𝑇 res 𝜈 . The figure is taken from [1]. very early time when 𝑇 ∼ 100 keV correspond… view at source ↗

read the original abstract

In this talk I discuss how neutrinos might help solving or alleviating different anomalies and tensions in cosmology. Invisible decays of the heaviest relic neutrinos might provide a way to solve the neutrino mass tension between cosmological observations and neutrino oscillation experiments. The excess radio background mystery could be explained by radiative decays of relic neutrinos. However, the upper bound on the neutrino effective magnetic moment requires some trick to be circumvented. To this extent, I discuss a recently proposed boomerang mechanism in which the visible sector throws dark neutrinos into the dark sector at $t \sim 100\,{\rm s}$ and $T \sim 100\,{\rm keV}$, and much later (basically at the present time) the dark sector throws back photons into the visible sector. The mechanism predicts an effective neutrino magnetic moment that might be within the reach of next experiments. Some contribution to the 21 cm cosmological signal is also expected. These are exciting times for cosmological searches of BSM physics.

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

This is a review talk synthesizing neutrino decay ideas for cosmological tensions, with the boomerang dark-sector sketch as the main organizing element but no new calculations.

read the letter

The main takeaway is that this talk reviews how invisible decays of the heaviest relic neutrinos could ease the tension between oscillation data and cosmological mass-sum bounds, while radiative decays via a recently proposed boomerang mechanism might account for the radio excess background. It also flags a possible contribution to the 21 cm signal and notes that the mechanism predicts an effective magnetic moment potentially reachable by future experiments. That synthesis is the useful part: it pulls several anomalies into one BSM neutrino-cosmology narrative without claiming to solve everything from scratch. The talk does a fair job of laying out the logic at a qualitative level and crediting the prior work on the boomerang idea. The soft spots are exactly where the stress-test note points. The boomerang requires neutrinos to be transferred into a hidden sector at t ~ 100 s and T ~ 100 keV, then photons returned at late times, all while generating a magnetic moment large enough to explain the excess yet small enough to satisfy existing limits. No Lagrangian, coupling values, decay rates, or consistency checks with BBN or CMB data are supplied, so it is impossible to judge whether the required dark-sector interactions can be arranged without new problems. The claims therefore rest on the mechanism working by construction rather than on demonstrated viability. This is aimed at people already working in neutrino cosmology who want a compact overview of these speculative links. It shows clear thinking in how the pieces fit together but does not contain the derivations or quantitative tests that would make it a primary research contribution. I would bring it to a reading group if the topic is BSM cosmology and tensions, but I would not cite it as a source of new results. It does not merit peer review as a standalone paper; it reads like a conference talk summary that would fit better in proceedings if that is the intended venue.

Referee Report

2 major / 1 minor

Summary. The manuscript discusses how neutrinos could alleviate cosmological tensions and anomalies: invisible decays of the heaviest relic neutrinos are proposed to resolve the neutrino mass tension between cosmology and oscillation data, while radiative decays via a 'boomerang' mechanism (transfer of neutrinos to a dark sector at t ~ 100 s and T ~ 100 keV, with photon return at late times) are suggested to explain the excess radio background. The mechanism is claimed to yield an effective neutrino magnetic moment within reach of future experiments and a contribution to the 21 cm signal.

Significance. If the mechanisms can be shown to be consistent with all bounds through explicit calculations, the ideas could offer a unified BSM neutrino explanation for multiple cosmological puzzles with testable predictions for magnetic moments and dark-sector effects. The work identifies potentially fruitful directions for connecting neutrino physics to cosmology, though its current qualitative nature limits immediate impact.

major comments (2)

[Boomerang mechanism] Boomerang mechanism (described in the main text following the abstract): no explicit Lagrangian, coupling constants, or decay-rate calculations are provided to demonstrate that the dark-sector transfer at T ~ 100 keV can occur without violating BBN constraints, overproducing invisible decays, or exceeding the current upper bound on the neutrino magnetic moment while still generating the required late-time photon flux to explain the radio excess.
[Invisible decays] Invisible decays proposal (main text): the assertion that decays of the heaviest relic neutrinos resolve the cosmological neutrino-mass tension is presented without any derivation, parameter scan, or consistency check against existing limits on neutrino lifetimes or the required suppression of the effective mass in cosmological observables.

minor comments (1)

The text refers to 'this talk' and 'I discuss,' indicating it is likely a proceedings summary of a presentation; for journal publication, rephrase to standard manuscript style and expand the qualitative sketches into at least schematic calculations.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the detailed and constructive report. The comments correctly identify the qualitative nature of the current presentation, which stems from its origin as a conference talk. We address each major point below and will revise the manuscript to incorporate additional details and references for improved rigor.

read point-by-point responses

Referee: [Boomerang mechanism] Boomerang mechanism (described in the main text following the abstract): no explicit Lagrangian, coupling constants, or decay-rate calculations are provided to demonstrate that the dark-sector transfer at T ~ 100 keV can occur without violating BBN constraints, overproducing invisible decays, or exceeding the current upper bound on the neutrino magnetic moment while still generating the required late-time photon flux to explain the radio excess.

Authors: We agree that the manuscript as written does not contain the explicit Lagrangian or rate calculations. These are provided in the original proposal paper on the boomerang mechanism, which we will cite explicitly. The couplings are chosen such that the visible-to-dark transfer occurs after BBN (T ~ 100 keV) with rates that avoid overproduction of invisible decays, remain below the current magnetic-moment bound, and produce the required late-time photon flux for the radio excess. In the revised version we will add a concise summary of the relevant Lagrangian terms, the key decay-rate expressions, and a brief consistency argument with BBN and existing bounds. revision: yes
Referee: [Invisible decays] Invisible decays proposal (main text): the assertion that decays of the heaviest relic neutrinos resolve the cosmological neutrino-mass tension is presented without any derivation, parameter scan, or consistency check against existing limits on neutrino lifetimes or the required suppression of the effective mass in cosmological observables.

Authors: The claim relies on prior literature in which invisible decays of the heaviest neutrino eigenstate suppress the effective mass inferred from cosmology while remaining compatible with oscillation data. We will revise the text to include a short derivation of the effective-mass suppression and cite the relevant lifetime bounds and parameter ranges that satisfy them. A full scan is beyond the scope of this talk-style manuscript, but the key consistency relations will be stated explicitly. revision: yes

Circularity Check

0 steps flagged

No internal derivation chain or self-referential reductions present

full rationale

The document is a conference talk that qualitatively discusses possible neutrino decay scenarios to address cosmological tensions, attributing the central 'boomerang mechanism' to a recently proposed idea without providing equations, Lagrangians, rate calculations, or parameter fits within this text. No load-bearing steps reduce by construction to inputs, self-citations, or ansatzes defined here; claims are presented as exploratory possibilities rather than derived predictions. The content is therefore self-contained as an overview without circularity.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 1 invented entities

The abstract invokes standard cosmological evolution and neutrino properties but introduces a dark sector transfer without independent evidence or derivation; no free parameters or explicit axioms are quantified.

axioms (1)

standard math Standard Big Bang cosmology and relic neutrino decoupling hold at T ~ 100 keV.
Implicit in the timing t ~ 100 s and T ~ 100 keV for the boomerang transfer.

invented entities (1)

Dark neutrinos in a hidden sector no independent evidence
purpose: To enable the boomerang transfer that circumvents magnetic moment bounds while producing observable photons later.
Postulated to solve the radio excess without direct evidence provided; independent_evidence false.

pith-pipeline@v0.9.0 · 5454 in / 1206 out tokens · 37114 ms · 2026-05-08T18:33:07.338540+00:00 · methodology

discussion (0)

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

IndisputableMonolith.Cost.FunctionalEquation washburn_uniqueness_aczel unclear

?

unclear
Relation between the paper passage and the cited Recognition theorem.

τ_{ν_i→ν_j+φ} ≃ 7×10^17 s · (0.05 eV/m_νi) · (10^-15/λ²_ij)²

What do these tags mean?

matches: The paper's claim is directly supported by a theorem in the formal canon.
supports: The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends: The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses: The paper appears to rely on the theorem as machinery.
contradicts: The paper's claim conflicts with a theorem or certificate in the canon.
unclear: Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Reference graph

Works this paper leans on

33 extracted references · 27 canonical work pages · 1 internal anchor

[1]

P.S.B.Dev,P.DiBari,I.Martínez-SolerandR.Roshan,Relicneutrinodecaysolutiontothe excess radio background, JCAP04(2024), 046 [arXiv:2312.03082 [hep-ph]]

work page arXiv 2024
[2]

B. Dev, P. Di Bari, I. Martinez-Soler and R. Roshan,Boomerang mechanism explaining the excess radio background, to appear in PRD, [arXiv:2509.03441 [hep-ph]]

work page arXiv
[3]

NuFit-6.0: Updated global analysis of three-flavor neutrino oscillations

I. Esteban, M. C. Gonzalez-Garcia, M. Maltoni, I. Martinez-Soler, J. P. Pinheiro and T.Schwetz,NuFit-6.0: updatedglobalanalysisofthree-flavorneutrinooscillations,JHEP12 (2024), 216 [arXiv:2410.05380 [hep-ph]]

work page internal anchor Pith review arXiv 2024
[4]

Astrophys

M. Tristram, A. J. Banday, M. Douspis, X. Garrido, K. M. Górski, S. Henrot-Versillé, L.T.Hergt,S.Ilić,R.KeskitaloandG.Lagache,etal.Cosmologicalparametersderivedfrom the final Planck data release (PR4), Astron. Astrophys.682(2024), A37 [arXiv:2309.10034 [astro-ph.CO]]. 11 How neutrinos could help solving cosmological anomalies and tensions

work page arXiv 2024
[5]

M.AbdulKarimetal.[DESI],DESIDR2results.II.Measurementsofbaryonacousticoscilla- tionsandcosmologicalconstraints,Phys.Rev.D112(2025)no.8,083515[arXiv:2503.14738 [astro-ph.CO]]

work page Pith review arXiv 2025
[6]

Giarè, O

W. Giarè, O. Mena, E. Specogna and E. Di Valentino,Neutrino mass tension or sup- pressed growth rate of matter perturbations?, Phys. Rev. D112(2025) no.10, 103520 [arXiv:2507.01848 [astro-ph.CO]]

work page arXiv 2025
[7]

S.HannestadandG.Raffelt,Constraininginvisibleneutrinodecayswiththecosmicmicrowave background, Phys. Rev. D72(2005), 103514 [arXiv:hep-ph/0509278 [hep-ph]]

work page arXiv 2005
[8]

P. D. Serpico,Cosmological Neutrino Mass Detection: The Best Probe of Neutrino Lifetime, Phys. Rev. Lett.98(2007), 171301 [arXiv:astro-ph/0701699 [astro-ph]]

work page arXiv 2007
[9]

M.ArchidiaconoandS.Hannestad,Updatedconstraintsonnon-standardneutrinointeractions from Planck, JCAP07(2014), 046 [arXiv:1311.3873 [astro-ph.CO]]

work page arXiv 2014
[10]

Escudero and M

M. Escudero and M. Fairbairn,Cosmological Constraints on Invisible Neutrino Decays Re- visited, Phys. Rev. D100(2019) no.10, 103531 [arXiv:1907.05425 [hep-ph]]

work page arXiv 2019
[11]

M.Escudero,J.Lopez-Pavon,N.RiusandS.Sandner,RelaxingCosmologicalNeutrinoMass Bounds with Unstable Neutrinos, JHEP12(2020), 119 [arXiv:2007.04994 [hep-ph]]

work page arXiv 2020
[12]

Craig, D

N. Craig, D. Green, J. Meyers and S. Rajendran,No𝜈s is Good News, JHEP09(2024), 097 [arXiv:2405.00836 [astro-ph.CO]]

work page arXiv 2024
[13]

D.J.Fixsen,TheTemperatureoftheCosmicMicrowaveBackground,Astrophys.J.707(2009), 916-920 [arXiv:0911.1955 [astro-ph.CO]]

work page arXiv 2009
[14]

Villela,et al

D.J.Fixsen,A.Kogut,S.Levin,M.Limon,P.Lubin,P.Mirel,M.Seiffert,J.Singal,E.Wollack and T. Villela,et al. ARCADE 2 Measurement of the Extra-Galactic Sky Temperature at 3-90 GHz, Astrophys. J.734(2011), 5 [arXiv:0901.0555 [astro-ph.CO]]

work page arXiv 2011
[15]

Lett.50(2024), 159-185 [arXiv:2408.01858 [astro-ph.HE]]

S.A.GrebenevandR.A.Sunyaev,IncreaseintheBrightnessoftheCosmicRadioBackground toward Galaxy Clusters, Astron. Lett.50(2024), 159-185 [arXiv:2408.01858 [astro-ph.HE]]

work page arXiv 2024
[16]

Chianese, P

M. Chianese, P. Di Bari, K. Farrag and R. Samanta,Probing relic neutrino radiative decays with 21 cm cosmology, Phys. Lett. B790(2019), 64-70 [arXiv:1805.11717 [hep-ph]]

work page arXiv 2019
[17]

Masso and R

E. Masso and R. Toldra,Photon spectrum produced by the late decay of a cosmic neutrino background, Phys. Rev. D60(1999), 083503 [arXiv:astro-ph/9903397 [astro-ph]]

work page arXiv 1999
[18]

Planck 2018 results. VI. Cosmological parameters

N. Aghanimet al.[Planck],Planck 2018 results. VI. Cosmological parameters, Astron. Astrophys.641(2020), A6 [erratum: Astron. Astrophys.652(2021), C4] [arXiv:1807.06209 [astro-ph.CO]]

work page Pith review arXiv 2018
[19]

Di Bari,Cosmology and the Early Universe, CRC Press, 2018, ISBN 978-1-4987-6170-3, 978-1-138-49690-3

P. Di Bari,Cosmology and the Early Universe, CRC Press, 2018, ISBN 978-1-4987-6170-3, 978-1-138-49690-3. 12 How neutrinos could help solving cosmological anomalies and tensions

2018
[20]

Dowell and G

J. Dowell and G. B. Taylor,The Radio Background Below 100 MHz, Astrophys. J. Lett.858 (2018) no.1, L9 [arXiv:1804.08581 [astro-ph.CO]]

work page arXiv 2018
[21]

R.N.MohapatraandP.B.Pal,Massiveneutrinosinphysicsandastrophysics.Secondedition, World Sci. Lect. Notes Phys.60(1998), 1-397

1998
[22]

Z. z. Xing and S. Zhou,Neutrinos in particle physics, astronomy and cosmology
[23]

A. G. Beda, V. B. Brudanin, V. G. Egorov, D. V. 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, [arXiv:1005.2736 [hep-ex]]

work page arXiv
[24]

G. G. Raffelt,New bound on neutrino dipole moments from globular cluster stars, Phys. Rev. Lett.64(1990), 2856-2858

1990
[25]

Enqvist, K

K. Enqvist, K. Kainulainen and J. Maalampi,Refraction and Oscillations of Neutrinos in the Early Universe, Nucl. Phys. B349(1991), 754-790

1991
[26]

Di Bari and R

P. Di Bari and R. Foot,Active sterile neutrino oscillations in the early universe: Asymmetry generationatlow|deltam**2|andtheLandau-Zenerapproximation,Phys.Rev.D65(2002), 045003 [arXiv:hep-ph/0103192 [hep-ph]]

work page arXiv 2002
[27]

D.AristizabalSierraandC.S.Fong,TheEDGESsignal: Animprintfromthemirrorworld?, Phys. Lett. B784(2018), 130-136 [arXiv:1805.02685 [hep-ph]]

work page arXiv 2018
[28]

R. Foot, M. J. Thomson and R. R. Volkas,Large neutrino asymmetries from neutrino oscilla- tions, Phys. Rev. D53(1996), R5349-R5353 [arXiv:hep-ph/9509327 [hep-ph]]

work page arXiv 1996
[29]

J. R. Pritchard and A. Loeb,21-cm cosmology, Rept. Prog. Phys.75(2012), 086901 [arXiv:1109.6012 [astro-ph.CO]]

work page Pith review arXiv 2012
[30]

J.608(2004), 622-635 [arXiv:astro-ph/0311514 [astro-ph]]

M.Zaldarriaga,S.R.FurlanettoandL.Hernquist,21Centimeterfluctuationsfromcosmicgas at high redshifts, Astrophys. J.608(2004), 622-635 [arXiv:astro-ph/0311514 [astro-ph]]

work page arXiv 2004
[31]

J.D.Bowman,A.E.E.Rogers,R.A.Monsalve,T.J.MozdzenandN.Mahesh,Anabsorption profilecentredat78megahertzinthesky-averagedspectrum,Nature555(2018)no.7694,67

2018
[32]

S.Singh,J.NambissanT.,R.Subrahmanyan,N.UdayaShankar,B.S.Girish,A.Raghunathan, R.Somashekar,K.S.SrivaniandM.SathyanarayanaRao,Onthedetectionofacosmicdawn signal in the radio background, Nature Astron.6(2022) no.5, 607-617 [arXiv:2112.06778 [astro-ph.CO]]

work page arXiv 2022
[33]

S.D. Bale, N. Bassett, J.O. Burns, J. Dorigo Jones, K. Goetz, C. Hellum-Bye et al., LuSEE ’Night’: The Lunar Surface Electromagnetics Experiment,arXiv e-prints(2023) arXiv:2301.10345 [2301.10345]. 13

work page arXiv 2023