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REVIEW 2 major objections 4 minor 48 references

DUNE can probe ultra-light neutrinophilic forces from a dark U(1)D sector and the same coupling that yields Hubble-relevant neutrino self-interactions.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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T0 review · grok-4.5

2026-07-11 19:09 UTC pith:7XNK6WLK

load-bearing objection Clean DUNE mapping of a known dark-neutrino portal onto long-range potentials and the Hubble-tension self-interaction window; solid enough to referee. the 2 major comments →

arxiv 2607.04441 v1 pith:7XNK6WLK submitted 2026-07-05 hep-ph hep-ex

Probing Neutrinophilic Long-Range Forces at DUNE

Sudip Jana , Pragyanprasu Swain This is my paper
classification hep-ph hep-ex
keywords dark neutrino portallong-range neutrino interactionsDUNEU(1)Dneutrino self-interactionsHubble tensionactive-sterile mixingneutrinophilic mediator
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The paper argues that a light dark sector charged under a new U(1)D gauge symmetry, which generates neutrino masses via an inverse-seesaw mechanism and communicates with the Standard Model only through active–dark neutrino mixing, produces ultra-long-range forces felt by neutrinos. Electrons and neutrons in the Earth, Moon, Sun, Milky Way and the cosmological matter distribution then induce flavor-dependent matter potentials that alter neutrino oscillation probabilities. Because DUNE has a 1285 km baseline and large matter effects, a ten-year exposure can place 3σ limits on these potentials at the 10^{-14} eV level (strongest in the eμ and eτ sectors). Mapping those limits onto the mediator-mass versus effective-coupling plane excludes previously unexplored territory down to geff ≲ 10^{-28} for masses around 10^{-35} eV. The identical parameters also generate non-standard neutrino self-interactions whose strength can reach 10^9–10^{10} GF—the range favored for delaying neutrino free-streaming and thereby easing the Hubble tension—while remaining consistent with existing oscillation data.

Core claim

With ten years of DUNE exposure the experiment can set 3σ upper bounds on the long-range potential of order 10^{-14} eV in the eμ and eτ sectors, thereby excluding previously unexplored regions of the (mZD, geff) plane down to geff ≲ 10^{-28} at mZD ∼ 10^{-35} eV; the same underlying active–dark mixing simultaneously produces neutrino self-interaction strengths G4 u_eff ∼ 10^9–10^{10} GF that are cosmologically relevant for the Hubble tension.

What carries the argument

The dark-neutrino portal under U(1)D: active–dark mixing induces an effective coupling of the ultra-light ZD mediator to ordinary matter (via Z–ZD mass mixing), generating a fully populated 3 imes3 flavor-space potential VLRI that is sourced by celestial neutron distributions and is directly linked to the four-neutrino self-interaction strength G4 u_eff.

Load-bearing premise

The mapping from oscillation limits to mediator parameters assumes that Earth, the Milky Way and the cosmological matter can be treated as continuous isoscalar distributions and that only the average potential at the detector needs to be computed, rather than the full path-dependent potential inside the Earth.

What would settle it

If DUNE’s measured uμ o u e appearance spectrum after ten years shows no deviation from standard three-flavor oscillations at the level that would be produced by a long-range potential of size ∼10^{-14} eV, the claimed sensitivity contours (and the overlapping Hubble-tension region) are ruled out.

Watch this falsifier — get emailed when new claim-graph text bears on it.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 4 minor

Summary. The paper studies a dark-neutrino portal under a new U(1)_D symmetry in which SM fields are neutral and right-handed (dark) neutrinos carry charge. Active–dark mixing induces an effective coupling of the light Z_D mediator to active neutrinos, generating both a flavor-structured matter potential (short-range NSI or long-range Yukawa) sourced by Earth/Moon/Sun/Milky-Way/cosmological neutrons and non-standard neutrino self-interactions. Using GLoBES with the DUNE TDR configuration (10 yr, equal u/ u-bar), the authors compute appearance probabilities and event spectra for three benchmark 2 imes2 flavor textures (eµ, e au, µ au), extract 3σ limits on the long-range potential VLRI ~ 10^{-14} eV, map them onto the (m_ZD, g_eff) plane down to g_eff ≲ 10^{-28} at m_ZD ~ 10^{-35} eV, and recast the same parameters into G_4 u_eff/G_F, showing overlap with the region preferred for alleviating the Hubble tension.

Significance. If the projected contours hold, the work supplies a concrete, experimentally accessible link between a well-motivated inverse-seesaw dark-sector model, long-baseline oscillation data, and cosmologically relevant neutrino self-interactions. The calculation rests on a standard GLoBES implementation of the summed Yukawa potential (Eqs. 11–12), a transparent Poisson abla^{2} with pulls and marginalization over heta23 and heta CP, and an explicit mapping (Eq. 14) that simultaneously constrains matter effects and NSSI. These features make the result falsifiable and useful for both the DUNE and early-Universe communities; the paper also correctly identifies previously unexplored regions of parameter space while remaining consistent with existing oscillation bounds.

major comments (2)
  1. [Matter potential and self-interactions of neutrinos] In the paragraph following Eq. 12 the authors state that only the average Earth potential evaluated at the detector is used, citing Refs. [27,33] for a full path-dependent treatment. For the ultra-light regime (m_ZD ≲ 10^{-20} eV) that drives the strongest claimed reach (g_eff ≲ 10^{-28}), the potential is essentially constant across the 1285 km baseline, so the average is an excellent proxy. Nevertheless, a short quantitative estimate of the residual bias for the intermediate-mass window 10^{-20}–10^{-12} eV (where the Yukawa range becomes comparable to the Earth radius) would strengthen the mapping of VLRI limits onto the (m_ZD, g_eff) plane shown in Fig. 6.
  2. [Projected Sensitivity of DUNE / Fig. 7] Fig. 7 and the surrounding text fix ε' = 10^{-3} when translating g_eff into G_4 u_eff/G_F via Eq. 14. Because ε' is an independent free parameter of the model (Eq. 6), the location of the Hubble-tension band relative to the DUNE contours is sensitive to this choice. A brief scan over a plausible range of ε' (or an explicit statement that the band simply rescales) is needed to make the claimed overlap robust.
minor comments (4)
  1. [Framework / Statistical methods] The three benchmark textures are clearly defined, but the text never states whether the relative phase of the off-diagonal U_α4U_β4* entries is marginalized or fixed to zero; a one-sentence clarification would remove ambiguity in the abla^{2} definition.
  2. [Oscillation probability and event spectra] Fig. 4 lower panels show event spectra but lack an explicit legend distinguishing signal from the various backgrounds listed in the DUNE TDR; adding it would improve readability.
  3. [Matter potential … Eq. 8] In Eq. 8 the factor 4c_W m_Z^{2}/g appears without a brief derivation from the Z–Z_D mass-mixing Lagrangian (Eq. 5); a short intermediate step would help non-specialist readers.
  4. [Appendix / Conclusions] The appendix reinterprets the limits in terms of |U_α4|^{2} under loop-induced mixing, but the main-text abstract and conclusions emphasize only the tree-level case; a single cross-reference would unify the presentation.

Circularity Check

0 steps flagged

No significant circularity: DUNE projected limits arise from independent GLoBES mock-data fits; self-citations supply only the model Lagrangian and prior applications, not the sensitivity contours themselves.

full rationale

The paper's central results are the 3σ VLRI bounds (Table I, ~10^{-14} eV) obtained by generating true events under the Standard Model (λ=0) and test events under the new potential, then minimizing the Poissonian χ² over θ23, δCP and systematics (Eqs. 15 and surrounding text). These are standard projected-sensitivity calculations; they do not recycle previously fitted constants. The mapping of VLRI onto the (m_ZD, g_eff) plane follows directly from the Yukawa potential (Eq. 11) summed over celestial sources (Eq. 12), and the further recast onto G4ν_eff/GF (Eq. 14, Fig. 7) is an algebraic translation that fixes ε′=10^{-3} by hand. Self-citations ([15,16] for the U(1)_D Lagrangian and inverse-seesaw mass matrix, [18,19] for earlier NSSI/Hubble remarks) introduce the framework and note phenomenological overlap, but the DUNE event spectra, probability engines, and χ² contours are computed afresh and do not reduce to those earlier numerical results. The Earth-potential averaging approximation is flagged by the authors themselves and does not create a definitional loop. No self-definitional identity, fitted-input-as-prediction, uniqueness theorem, or ansatz smuggling is present. Score 1 reflects only the ordinary presence of non-load-bearing self-citations for model setup.

Axiom & Free-Parameter Ledger

4 free parameters · 4 axioms · 2 invented entities

The central sensitivity claims rest on a specific dark-sector model (U(1)D charged right-handed neutrinos, inverse-seesaw mass generation, tree-level Z–ZD mass mixing) together with standard oscillation parameters and idealized celestial matter distributions. Free parameters are the mediator mass, effective coupling and active-sterile mixings; the invented entities are the dark gauge boson and the dark neutrinos themselves.

free parameters (4)
  • m_ZD
    Mediator mass scanned from 10^{-35} eV to 10^{12} eV; free continuous parameter that sets the interaction range.
  • g_eff
    Effective coupling g_D ε′ U*α4 Uβ4; free continuous parameter that sets the strength of both the long-range potential and the self-interaction.
  • ε′
    Z–ZD mass-mixing parameter, fixed to 10^{-3} when mapping to self-interactions; otherwise free.
  • |Uα4|
    Active-sterile mixing elements that define the three benchmark flavor textures; free within experimental bounds.
axioms (4)
  • domain assumption Standard three-flavor oscillation Hamiltonian plus SM charged-current matter potential VCC = √2 GF ne
    Used throughout the probability engine; taken from NuFIT 5.1 best-fit values.
  • domain assumption Celestial matter distributions are electrically neutral and (except Sun and cosmology) isoscalar; Earth potential is replaced by its average at the detector
    Stated in the long-range potential section; simplifies the multi-source sum VLRI.
  • domain assumption Kinetic mixing contribution vanishes in static unpolarized neutral matter; only mass mixing generates the potential
    Explicitly used to drop the ε term in Eq. (8).
  • ad hoc to paper Normal mass ordering and fixed solar/atmospheric parameters except θ23, δCP
    Chosen for the true and test spectra; inverted ordering not scanned.
invented entities (2)
  • U(1)D dark gauge boson ZD no independent evidence
    purpose: Mediates both the long-range neutrino-matter potential and the four-neutrino self-interaction
    Introduced via the dark-neutrino portal Lagrangian; mass and coupling are free parameters of the model.
  • Dark neutrinos ND (right-handed neutrinos charged under U(1)D) no independent evidence
    purpose: Generate active-sterile mixing that transmits the dark force to ordinary neutrinos and realize the inverse seesaw
    Core of the framework taken from earlier papers by overlapping authors; no direct detection claimed here.

pith-pipeline@v1.1.0-grok45 · 18984 in / 2825 out tokens · 30876 ms · 2026-07-11T19:09:01.605621+00:00 · methodology

0 comments
read the original abstract

Neutrino oscillations provide compelling evidence for physics beyond the Standard Model, while the weakly interacting nature of neutrinos makes them powerful probes of new interactions and hidden sectors. In this work, we investigate a \textit{dark neutrino portal} scenario in which neutrino mass generation is linked to a light dark sector charged under a new $U(1)_D$ gauge symmetry. While Standard Model fields remain neutral under $U(1)_D$, the dark neutrino sector is charged and communicates with the Standard Model exclusively through active--dark neutrino mixing. The associated neutrinophilic mediator induces ultra-long-range interactions, whereby electrons and neutrons in the Earth, Moon, Sun, Milky Way, and the cosmological matter distribution generate sizable matter potentials that modify neutrino oscillations. We explore the sensitivity of the upcoming Deep Underground Neutrino Experiment (DUNE), whose long baseline and pronounced matter effects make it uniquely suited to probe such interactions. We show that DUNE can access previously unexplored regions of parameter space and demonstrate that the same underlying coupling can simultaneously give rise to sizable neutrino self-interactions, including regions relevant for alleviating the Hubble tension, while remaining consistent with current neutrino oscillation constraints.

Figures

Figures reproduced from arXiv: 2607.04441 by Pragyanprasu Swain, Sudip Jana.

Figure 1
Figure 1. Figure 1: FIG. 1. Schematic representation of DUNE long-baseline neu [PITH_FULL_IMAGE:figures/full_fig_p001_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. Feynman diagram depicting the interaction between [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3. The Feynman diagram representing the neutrino self [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4. Neutrino oscillation probabilities and event spectra at DUNE in the presence of the dark gauge boson-induced [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5. Projected limits on the new physics potential in the [PITH_FULL_IMAGE:figures/full_fig_p007_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6. Projected sensitivity on the mass vs coupling plane of the new light mediator from [PITH_FULL_IMAGE:figures/full_fig_p008_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: FIG. 7. Projected 3 [PITH_FULL_IMAGE:figures/full_fig_p009_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: FIG. 8. The Feynman diagram showing the loop-induced neutrino-matter interactions. [PITH_FULL_IMAGE:figures/full_fig_p010_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: FIG. 9. Translated upper limits (derived from Fig. [PITH_FULL_IMAGE:figures/full_fig_p011_9.png] view at source ↗

discussion (0)

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Reference graph

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