arxiv: 2605.06777 · v1 · submitted 2026-05-07 · ✦ hep-ph · astro-ph.HE· hep-ex

Recognition: no theorem link

Neutrino-Antineutrino Conversion from Ultralight Vector Dark Matter

Asher Berlin , Rodolfo Capdevilla , Ting Cheng , Matheus Hostert , Pedro A. N. Machado

Authors on Pith no claims yet

Pith reviewed 2026-05-11 00:55 UTC · model grok-4.3

classification ✦ hep-ph astro-ph.HEhep-ex

keywords neutrino-antineutrino conversionultralight vector dark matterU(1) B-LMajorana neutrinossupernova neutrinosDUNE Hyper-Kamiokande JUNOlepton number violation

0 comments

The pith

Majorana neutrinos convert to antineutrinos in an ultralight vector dark matter background, enabling supernova observations to test gauge couplings down to 10^{-32}.

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

The paper shows that if neutrinos are Majorana particles, an ultralight vector boson carrying lepton number can drive coherent flips from neutrinos to antineutrinos. The flip amplitude is suppressed by the tiny neutrino mass, yet the long distance from the Sun or a supernova multiplies the effect into an observable signal. Detectors watching a galactic supernova burst could therefore set limits on the dark matter coupling strength that reach far below the reach of other planned experiments. A reader cares because the same data collected for neutrino astrophysics would simultaneously test a new dark matter candidate and the fundamental nature of neutrinos.

Core claim

In a coherent background of ultralight vector dark matter coupled to lepton number, Majorana neutrinos undergo neutrino-to-antineutrino conversion. The conversion is suppressed by the small neutrino mass but enhanced by long astrophysical baselines, so that solar neutrinos and especially supernova neutrino bursts at DUNE, Hyper-Kamiokande, and JUNO can probe U(1)_{B-L} gauge couplings as small as 10^{-32} to 10^{-25} for dark matter masses between 10^{-22} eV and 10^{-14} eV.

What carries the argument

Coherent neutrino-antineutrino oscillation driven by the ultralight vector boson background, whose oscillation frequency is set by the dark matter mass and whose amplitude grows with the gauge coupling and baseline length.

If this is right

Supernova neutrino data would simultaneously constrain dark matter parameters and test whether neutrinos are Majorana particles.
Solar neutrino fluxes could exhibit a small but steady conversion signature at lower energies.
The mechanism distinguishes U(1)_{B-L} or U(1)_{L_i-L_j} dark matter from other ultralight candidates that do not couple to lepton number.
Existing or near-future neutrino detectors gain sensitivity to a previously inaccessible dark matter mass range.

Where Pith is reading between the lines

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

The same background could induce time-varying signals if the dark matter field oscillates, offering a potential time-domain search strategy.
In the early universe the conversion effect might alter neutrino decoupling or big-bang nucleosynthesis in ways that future cosmological data could test.
Analogous conversions might appear in other environments with high neutrino density, such as neutron star mergers.

Load-bearing premise

Neutrinos must be Majorana fermions so that the dark matter interaction can produce a conversion term between neutrino and antineutrino states.

What would settle it

A galactic supernova burst recorded at DUNE, Hyper-Kamiokande, or JUNO showing no excess antineutrino events above standard expectations in the predicted mass and coupling window.

Figures

Figures reproduced from arXiv: 2605.06777 by Asher Berlin, Matheus Hostert, Pedro A. N. Machado, Rodolfo Capdevilla, Ting Cheng.

read the original abstract

We show that Majorana neutrinos convert into antineutrinos in a background of ultralight vector dark matter coupled to lepton number, such as the gauge boson of $\text{U}(1)_{B-L}$ or $\text{U}(1)_{L_i - L_j}$ with $i, j = e , \mu, \tau$. This effect is suppressed by the small neutrino mass, but the enhancement by long astrophysical baselines can enable future searches for solar and supernova neutrinos to explore uncharted parameter space. For instance, for $\text{U}(1)_{B-L}$ dark matter, the observation of a supernova neutrino burst at DUNE, Hyper-Kamiokande, and JUNO could probe gauge couplings as small as $e^\prime \sim 10^{-32} - 10^{-25}$ for dark matter masses of $m_{A^\prime} \sim 10^{-22} \ \text{eV} - 10^{-14} \ \text{eV}$, beyond the capability of other future probes.

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 / 2 minor

Summary. The paper claims that Majorana neutrinos undergo conversion to antineutrinos in a coherent background of ultralight vector dark matter coupled to lepton number (e.g., the gauge boson A' of U(1)_{B-L} or U(1)_{L_i-L_j}). Although suppressed by the small neutrino mass, the effect is enhanced over long astrophysical baselines, enabling future detectors (DUNE, Hyper-Kamiokande, JUNO) to probe gauge couplings e' as small as 10^{-32}–10^{-25} for m_{A'} in the range 10^{-22}–10^{-14} eV via supernova neutrino bursts.

Significance. If the central derivation holds, the result would open a new probe of ultralight vector dark matter using neutrino astronomy, reaching couplings orders of magnitude below other planned searches and illustrating the leverage of coherence over Gpc-scale baselines. The sensitivity projections for specific experiments constitute a concrete, falsifiable prediction.

major comments (1)

[Formalism section deriving the effective Hamiltonian] The interaction Lagrangian is written as e' A'_μ J^μ with J^μ = ν-bar γ^μ ν (see the formalism section deriving the effective Hamiltonian). For Majorana neutrinos this vector current vanishes identically by the self-conjugate property ψ = ψ^c. Consequently the classical ultralight DM background generates no potential or mixing term, rendering the claimed ν ↔ ν-bar conversion probability zero independent of baseline length or coherence. This is load-bearing for the entire sensitivity claim.

minor comments (2)

[Abstract] The abstract quotes numerical sensitivity ranges without stating the assumed DM density, coherence length, or supernova neutrino spectrum used to obtain them; these should be made explicit.
[Throughout the manuscript] Notation for the dark-matter field alternates between A' and A'_μ; adopt a single consistent symbol throughout.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their careful reading and the detailed comment on the formalism. We address the point below and will revise the manuscript to resolve the issue.

read point-by-point responses

Referee: [Formalism section deriving the effective Hamiltonian] The interaction Lagrangian is written as e' A'_μ J^μ with J^μ = ν-bar γ^μ ν (see the formalism section deriving the effective Hamiltonian). For Majorana neutrinos this vector current vanishes identically by the self-conjugate property ψ = ψ^c. Consequently the classical ultralight DM background generates no potential or mixing term, rendering the claimed ν ↔ ν-bar conversion probability zero independent of baseline length or coherence. This is load-bearing for the entire sensitivity claim.

Authors: We thank the referee for this observation. We agree that for a Majorana neutrino field the vector current vanishes identically, so the interaction Lagrangian term as written generates no classical potential or mixing from the ultralight vector DM background. This renders the conversion probability zero and affects the central claim. We will revise the formalism section to correct the derivation, either by reformulating the model with Dirac neutrinos (treating the Majorana mass as a small perturbation) or by deriving the appropriate effective couplings consistent with Majorana statistics. The revised version will contain an updated effective Hamiltonian and, if needed, adjusted sensitivity projections. This revision directly addresses the load-bearing concern. revision: yes

Circularity Check

0 steps flagged

No significant circularity; derivation is self-contained from Lagrangian.

full rationale

The paper derives the conversion probability directly from the interaction Lagrangian term for the ultralight vector DM background acting on neutrinos, using standard effective Hamiltonian evolution over long baselines. This leads to the quoted sensitivity reach for supernova neutrinos at DUNE/Hyper-K/JUNO without any fitted parameters being renamed as predictions, without load-bearing self-citations for uniqueness theorems, and without definitional loops where the output is presupposed in the input. The Majorana assumption is stated upfront and the calculation proceeds from the given model; any debate over whether the vector current vanishes is a question of model validity rather than circularity in the derivation chain. The result is independent of the target parameter space claims.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 1 invented entities

The claim rests on the Majorana nature of neutrinos and the existence of an ultralight vector boson as dark matter; the gauge coupling and mass are free parameters to be constrained rather than fitted.

free parameters (2)

gauge coupling e'
Free parameter whose small values are probed by the supernova signal.
dark matter mass m_A'
Free parameter scanned over the ultralight range 10^{-22} to 10^{-14} eV.

axioms (2)

domain assumption Neutrinos are Majorana fermions
Required for the conversion process to occur as stated.
ad hoc to paper Ultralight vector boson constitutes dark matter and couples to lepton number
Postulated extension of the Standard Model.

invented entities (1)

Ultralight vector dark matter A' no independent evidence
purpose: Induces coherent neutrino-antineutrino conversion via lepton-number coupling
New postulated dark matter candidate with specific mass and coupling range.

pith-pipeline@v0.9.0 · 5497 in / 1413 out tokens · 62261 ms · 2026-05-11T00:55:59.559893+00:00 · methodology

discussion (0)

Reference graph

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