pith. sign in

arxiv: 2606.17132 · v1 · pith:EFILZXBVnew · submitted 2026-06-15 · ✦ hep-ph · astro-ph.HE· hep-ex· hep-th· nucl-th

Are neutrinos Majorana? Fixed-target and high-energy astrophysical searches decide

Gabriela Barenboim , Mauricio Bustamante , Qinrui Liu This is my paper

Pith reviewed 2026-06-27 03:15 UTC · model grok-4.3

classification ✦ hep-ph astro-ph.HEhep-exhep-thnucl-th
keywords Majorana neutrinosDirac neutrinosheavy neutral leptonsSHiP experimentneutrino telescopesflavor mixingastrophysical neutrinosneutrinoless double beta decay
0
0 comments X

The pith

Heavy neutral leptons can reveal whether neutrinos are Majorana by inducing a detectable flavor shift in astrophysical neutrinos.

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 heavy neutral lepton would cause a shift in the flavor composition of high-energy astrophysical neutrinos only if neutrinos are Majorana fermions. This shift can be observed by neutrino telescopes at TeV to PeV energies, independent of the source flavor composition. Meanwhile, the SHiP experiment can discover such an HNL and measure its mixing parameters with active neutrinos. Because the effect is prominent in the muon and tau sectors, it avoids the limitations of neutrinoless double beta decay searches. A joint detection would confirm the Majorana nature, while its absence would favor Dirac neutrinos.

Core claim

A heavy neutral lepton triggers a high-energy shift in active neutrino flavor mixing only if the neutrinos are Majorana. For GeV-scale HNLs, SHiP can discover the HNL and its mixing, while scattering of TeV-PeV astrophysical neutrinos reveals the resulting flavor shift at Earth, detectable regardless of source composition. This provides a probe sensitive to muon and tau sectors.

What carries the argument

Heavy neutral lepton (HNL) inducing high-energy shift in active neutrino flavor mixing, observable only for Majorana neutrinos.

If this is right

  • Discovery of GeV-scale HNL at SHiP with measured mixing to active flavors.
  • Detection of altered flavor ratios in astrophysical neutrinos by telescopes.
  • The flavor shift bypasses electron-only blind spots of 0νββ decay.
  • Correlated signals would establish neutrinos as Majorana particles.
  • Lack of correlated signals would indicate Dirac neutrinos.

Where Pith is reading between the lines

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

  • This method links laboratory fixed-target experiments with high-energy astrophysics in a new way.
  • It could be extended to other high-energy neutrino sources or experiments.
  • If neutrinos are Majorana, this might constrain the scale of new physics beyond the standard model.
  • Future improvements in flavor resolution at telescopes would enhance the test.

Load-bearing premise

The high-energy flavor mixing shift triggered by the HNL occurs exclusively when neutrinos are Majorana and can be distinguished in astrophysical scattering despite unknown source flavors.

What would settle it

Finding an HNL at SHiP whose mixing would predict a flavor shift but observing no such shift in astrophysical neutrino data, or observing the shift without an HNL at SHiP.

Figures

Figures reproduced from arXiv: 2606.17132 by Gabriela Barenboim, Mauricio Bustamante, Qinrui Liu.

Figure 1
Figure 1. Figure 1: FIG. 1 [PITH_FULL_IMAGE:figures/full_fig_p001_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2 [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3 [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4 [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5 [PITH_FULL_IMAGE:figures/full_fig_p009_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6 [PITH_FULL_IMAGE:figures/full_fig_p011_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: FIG. 7 [PITH_FULL_IMAGE:figures/full_fig_p014_7.png] view at source ↗
Figure 9
Figure 9. Figure 9: FIG. 9 [PITH_FULL_IMAGE:figures/full_fig_p016_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: FIG. 10 [PITH_FULL_IMAGE:figures/full_fig_p017_10.png] view at source ↗
Figure 12
Figure 12. Figure 12: FIG. 12 [PITH_FULL_IMAGE:figures/full_fig_p019_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: shows R as a function of |UαN | 2/|UeN | 2 and M plane (α = µ, τ ). We identify three distinct regions: R ≪ 1: The 0νββ mass is sensitive, astrophysical neutrinos are insensitive. The 0νββ mass is dominantly sensitive to an HNL when |UeN | 2 ≫ |UµN | 2 , |UτN | 2 , i.e., in [PITH_FULL_IMAGE:figures/full_fig_p021_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: FIG. 14 [PITH_FULL_IMAGE:figures/full_fig_p026_14.png] view at source ↗
Figure 15
Figure 15. Figure 15: FIG. 15 [PITH_FULL_IMAGE:figures/full_fig_p027_15.png] view at source ↗
Figure 16
Figure 16. Figure 16: FIG. 16 [PITH_FULL_IMAGE:figures/full_fig_p029_16.png] view at source ↗
read the original abstract

Determining whether the neutrino is a Dirac or Majorana fermion remains a fundamental open question. Conventional searches rely on neutrinoless double beta decay, but this electron-only channel suffers from blind spots. We propose a new, complementary probe to overcome this limitation. A heavy neutral lepton (HNL) triggers a high-energy shift in how the active neutrino flavors ($\nu_e$, $\nu_\mu$, $\nu_\tau$) mix -- but only if the neutrinos are Majorana. For GeV-scale HNLs, the upcoming beam-dump experiment SHiP can discover the HNL and measure how it mixes with the active flavors. Separately, the scattering of TeV--PeV astrophysical neutrinos can resolve the HNL, revealing a shift in the proportions of each flavor arriving at Earth that could be detected by neutrino telescopes, regardless of the unknown flavor composition at the astrophysical neutrino sources. Because this flavor shift is most sensitive to the muon and tau sectors, it bypasses the blind spots of neutrinoless double beta decay. A correlated signal at SHiP and next-generation neutrino telescopes would prove that neutrinos are Majorana; its absence would point to them being Dirac.

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 / 0 minor

Summary. The manuscript proposes that a GeV-scale heavy neutral lepton (HNL) induces a high-energy shift in active-neutrino flavor mixing only if neutrinos are Majorana. Discovery and mixing measurements of the HNL at the SHiP beam-dump experiment, combined with detection of the resulting shift in TeV–PeV astrophysical neutrino flavor ratios at next-generation telescopes, would establish the Majorana nature; absence of the correlated signal would indicate Dirac neutrinos. The effect is claimed to be observable in the muon and tau sectors and independent of unknown source flavor composition, thereby complementing neutrinoless double-beta decay.

Significance. If the central mechanism is quantitatively validated, the proposal supplies a genuinely new, multi-messenger test of the Dirac/Majorana question that is sensitive to flavor sectors inaccessible to 0νββ decay. The correlated-signal logic is falsifiable in principle and leverages existing or near-term experimental capabilities (SHiP and IceCube-Gen2/KM3NeT-class telescopes).

major comments (1)
  1. [Abstract / mechanism description] Abstract and mechanism section: the load-bearing claim that the HNL-induced flavor-ratio deviation remains detectable 'regardless of the unknown flavor composition at the astrophysical neutrino sources' requires explicit demonstration that the shift vector in (e:μ:τ) space lies outside the manifold spanned by all plausible source ratios (pion-decay, muon-damped, neutron-decay, etc.) after standard oscillations. No mixing-matrix calculation, deviation magnitude, or comparison against source-variation span is provided, leaving the independence assertion unverified.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for the careful reading, the positive assessment of the proposal's significance, and the constructive comment. We respond to the major comment below.

read point-by-point responses

  1. Referee: [Abstract / mechanism description] Abstract and mechanism section: the load-bearing claim that the HNL-induced flavor-ratio deviation remains detectable 'regardless of the unknown flavor composition at the astrophysical neutrino sources' requires explicit demonstration that the shift vector in (e:μ:τ) space lies outside the manifold spanned by all plausible source ratios (pion-decay, muon-damped, neutron-decay, etc.) after standard oscillations. No mixing-matrix calculation, deviation magnitude, or comparison against source-variation span is provided, leaving the independence assertion unverified.

    Authors: We agree that an explicit demonstration is required to substantiate the independence claim. In the revised manuscript we will add a dedicated calculation (in the mechanism section or a new appendix) that computes the HNL-induced shift vector in flavor space, quantifies its magnitude for GeV-scale HNL parameters, and explicitly compares it to the span of variations arising from standard source compositions (pion-decay, muon-damped, neutron-decay) after vacuum oscillations. This will verify that the shift lies outside the source-variation manifold and remains detectable. revision: yes

Circularity Check

0 steps flagged

No significant circularity; proposal is self-contained

full rationale

The paper proposes a new observational strategy that correlates HNL discovery at SHiP with high-energy astrophysical neutrino flavor measurements to distinguish Majorana from Dirac neutrinos. This relies on standard BSM extensions and external experimental capabilities rather than any internal fitting, self-referential definitions, or load-bearing self-citations. No equations or predictions in the provided text reduce to inputs by construction, and the central claim remains independent of the paper's own fitted values or prior author work invoked as an unverified uniqueness theorem.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The proposal assumes standard extensions of the Standard Model with heavy neutral leptons that mix with active neutrinos only under Majorana conditions; no new free parameters or invented entities are introduced in the abstract.

axioms (2)
  • domain assumption Neutrinos can be either Dirac or Majorana fermions
    Fundamental open question stated in the abstract.
  • domain assumption Heavy neutral leptons mix with active neutrino flavors and induce flavor shifts only for Majorana neutrinos
    Core mechanism invoked for the proposed signal.

pith-pipeline@v0.9.1-grok · 5757 in / 1240 out tokens · 47227 ms · 2026-06-27T03:15:50.734545+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

167 extracted references · 1 canonical work pages

  1. [1]

    Majorana, Teoria simmetrica dell’elettrone e del positrone, Nuovo Cim.14, 171 (1937)

    E. Majorana, Teoria simmetrica dell’elettrone e del positrone, Nuovo Cim.14, 171 (1937)

    1937

  2. [2]

    R. N. Mohapatra and A. Y. Smirnov, Neutrino Mass and New Physics, Ann. Rev. Nucl. Part. Sci.56, 569 (2006), arXiv:hep-ph/0603118

    Pith/arXiv arXiv 2006

  3. [3]

    S. F. King, Right-handed neutrinos: seesaw models and signatures (2025) arXiv:2502.07877 [hep-ph]. 31

    arXiv 2025

  4. [4]

    W. H. Furry, On transition probabilities in double beta- disintegration, Phys. Rev.56, 1184 (1939)

    1939

  5. [5]

    Agostini, G

    M. Agostini, G. Benato, J. A. Detwiler, J. Men´ endez, and F. Vissani, Toward the discovery of matter creation with neutrinolessββdecay, Rev. Mod. Phys.95, 025002 (2023), arXiv:2202.01787 [hep-ex]

    arXiv 2023

  6. [6]

    Pascoli and S

    S. Pascoli and S. T. Petcov, Majorana neutrinos, neu- trino mass spectrum, CP violation and neutrinoless dou- ble beta decay. I. The three neutrino mixing case, Phys. Rev. D68, 093007 (2003), arXiv:hep-ph/0308034

    Pith/arXiv arXiv 2003

  7. [7]

    SHiP Collaboration, Sensitivity of the SHiP exper- iment to Heavy Neutral Leptons, JHEP04, 077, arXiv:1811.00930

    Pith/arXiv arXiv

  8. [8]

    Grimus and L

    W. Grimus and L. Lavoura, Renormalization of the neu- trino mass operators in the multi-Higgs-doublet stan- dard model, Eur. Phys. J. C39, 219 (2005), arXiv:hep- ph/0409231

    arXiv 2005

  9. [9]

    Aristizabal Sierra and C

    D. Aristizabal Sierra and C. E. Yaguna, On the impor- tance of the 1-loop finite corrections to seesaw neutrino masses, JHEP08, 013, arXiv:1106.3587 [hep-ph]

    Pith/arXiv arXiv

  10. [10]

    Abbasiet al., Characterization of the Three- Flavor Composition of Cosmic Neutrinos with IceCube, (2025), arXiv:2510.24957 [astro-ph.HE]

    R. Abbasiet al., Characterization of the Three- Flavor Composition of Cosmic Neutrinos with IceCube, (2025), arXiv:2510.24957 [astro-ph.HE]

    arXiv 2025

  11. [11]

    N. Song, S. W. Li, C. A. Arg¨ uelles, M. Bustamante, and A. C. Vincent, The future of high-energy astro- physical neutrino flavor measurements, JCAP04, 054, arXiv:2012.12893 [hep-ph]

    arXiv 2012

  12. [12]

    Bustamante, Q

    M. Bustamante, Q. Liu, and G. Barenboim, Astrophys- ical bounds on the high-energy evolution of neutrino mixing, (2026), arXiv:2604.14409 [hep-ph]

    Pith/arXiv arXiv 2026

  13. [13]

    Bustamante, Q

    M. Bustamante, Q. Liu, and G. Barenboim, Measuring neutrino mixing above 1 TeV with astrophysical neutri- nos, (2026), arXiv:2602.14308 [hep-ph]

    arXiv 2026

  14. [14]

    Weinberg, Baryon and Lepton Nonconserving Pro- cesses, Phys

    S. Weinberg, Baryon and Lepton Nonconserving Pro- cesses, Phys. Rev. Lett.43, 1566 (1979)

    1979

  15. [15]

    E. E. Jenkins, A. V. Manohar, and M. Trott, Renor- malization group evolution of the standard model di- mension six operators I: Formalism and Lambda depen- dence, JHEP10, 087, arXiv:1308.2627 [hep-ph]

    arXiv

  16. [16]

    Navaset al.(Particle Data Group), Review of particle physics, Phys

    S. Navaset al.(Particle Data Group), Review of particle physics, Phys. Rev. D110, 030001 (2024)

    2024

  17. [17]

    P. F. de Salas, D. V. Forero, S. Gariazzo, P. Mart´ ınez- Mirav´ e, O. Mena, C. A. Ternes, M. T´ ortola, and J. W. F. Valle, 2020 global reassessment of the neutrino oscillation picture, JHEP02, 071, arXiv:2006.11237 [hep-ph]

    Pith/arXiv arXiv 2020

  18. [18]

    Capozzi, E

    F. Capozzi, E. Di Valentino, E. Lisi, A. Marrone, A. Melchiorri, and A. Palazzo, Unfinished fabric of the three neutrino paradigm, Phys. Rev. D104, 083031 (2021), arXiv:2107.00532 [hep-ph]

    arXiv 2021

  19. [19]

    Esteban, M

    I. Esteban, M. C. Gonz´ alez-Garc´ ıa, M. Maltoni, I. Mart´ ınez-Soler, J. P. Pinheiro, and T. Schwetz, Nu- Fit 6.0: updated global analysis of three-flavor neutrino oscillations, JHEP12, 216, arXiv:2410.05380 [hep-ph]

    Pith/arXiv arXiv

  20. [20]

    B. Abiet al.(DUNE), Deep Underground Neutrino Ex- periment (DUNE), Far Detector Technical Design Re- port, Volume I Introduction to DUNE, JINST15(08), T08008, arXiv:2002.02967 [physics.ins-det]

    arXiv 2002

  21. [21]

    Abeet al.(Hyper-Kamiokande), Hyper-Kamiokande Design Report, (2018), arXiv:1805.04163 [physics.ins- det]

    K. Abeet al.(Hyper-Kamiokande), Hyper-Kamiokande Design Report, (2018), arXiv:1805.04163 [physics.ins- det]

    Pith/arXiv arXiv 2018

  22. [22]

    Bondarenko, A

    K. Bondarenko, A. Boyarsky, D. Gorbunov, and O. Ruchayskiy, Phenomenology of GeV-scale Heavy Neutral Leptons, JHEP11, 032, arXiv:1805.08567 [hep- ph]

    Pith/arXiv arXiv

  23. [23]

    de Blas, M

    J. de Blas, M. Chala, and J. Santiago, Global Con- straints on Lepton-Quark Contact Interactions, Phys. Rev. D88, 095011 (2013), arXiv:1307.5068 [hep-ph]

    Pith/arXiv arXiv 2013

  24. [24]

    Fern´ andez-Mart´ ınez, M

    E. Fern´ andez-Mart´ ınez, M. Gonz´ alez-L´ opez, J. Hern´ andez-Garc´ ıa, M. Hostert, and J. L´ opez- Pav´ on, Effective portals to heavy neutral leptons, JHEP09, 001, arXiv:2304.06772 [hep-ph]

    arXiv

  25. [25]

    Fern´ andez-Mart´ ınez, M

    E. Fern´ andez-Mart´ ınez, M. Gonz´ alez-L´ opez, J. Hern´ andez-Garc´ ıa, M. Hostert, and J. L´ opez- Pav´ on, Heavy-Neutrino-Limits,https://github.com/ mhostert/Heavy-Neutrino-Limits(2026)

    2026

  26. [26]

    S. H. Margolis, D. N. Schramm, and R. Silberberg, Ultrahigh-Energy Neutrino Astronomy, Astrophys. J. 221, 990 (1978)

    1978

  27. [27]

    F. W. Stecker, Diffuse Fluxes of Cosmic High-Energy Neutrinos, Astrophys. J.228, 919 (1979)

    1979

  28. [28]

    S. R. Kelner, F. A. Aharonian, and V. V. Bugayov, Energy spectra of gamma-rays, electrons and neutrinos produced at proton-proton interactions in the very high energy regime, Phys. Rev. D74, 034018 (2006), [Er- ratum: Phys. Rev. D 79, 039901 (2009)], arXiv:astro- ph/0606058

    arXiv 2006

  29. [29]

    M¨ ucke, R

    A. M¨ ucke, R. Engel, J. P. Rachen, R. J. Protheroe, and T. Stanev, SOPHIA: Monte Carlo simulations of photohadronic processes in astrophysics, Comput. Phys. Commun.124, 290 (2000), arXiv:astro-ph/9903478

    Pith/arXiv arXiv 2000

  30. [30]

    S. R. Kelner and F. A. Aharonian, Energy spectra of gamma-rays, electrons and neutrinos produced at in- teractions of relativistic protons with low energy ra- diation, Phys. Rev. D78, 034013 (2008), [Erratum: Phys. Rev. D 82, 099901 (2010)], arXiv:0803.0688 [astro-ph]

    Pith/arXiv arXiv 2008

  31. [31]

    H¨ ummer, M

    S. H¨ ummer, M. Ruger, F. Spanier, and W. Win- ter, Simplified models for photohadronic interactions in cosmic accelerators, Astrophys. J.721, 630 (2010), arXiv:1002.1310 [astro-ph.HE]

    Pith/arXiv arXiv 2010

  32. [32]

    Abbasiet al.(IceCube), Observation of high-energy neutrinos from the Galactic plane, Science380, adc9818 (2023), arXiv:2307.04427 [astro-ph.HE]

    R. Abbasiet al.(IceCube), Observation of high-energy neutrinos from the Galactic plane, Science380, adc9818 (2023), arXiv:2307.04427 [astro-ph.HE]

    arXiv 2023

  33. [33]

    Kashti and E

    T. Kashti and E. Waxman, Flavoring astrophysical neu- trinos: Flavor ratios depend on energy, Phys. Rev. Lett. 95, 181101 (2005), arXiv:astro-ph/0507599

    Pith/arXiv arXiv 2005

  34. [34]

    Kachelrieß, S

    M. Kachelrieß, S. Ostapchenko, and R. Tom` as, High energy neutrino yields from astrophysical sources. 2. Magnetized sources, Phys. Rev. D77, 023007 (2008), arXiv:0708.3047 [astro-ph]

    Pith/arXiv arXiv 2008

  35. [35]

    Lipari, M

    P. Lipari, M. Lusignoli, and D. Meloni, Flavor Compo- sition and Energy Spectrum of Astrophysical Neutrinos, Phys. Rev. D75, 123005 (2007), arXiv:0704.0718 [astro- ph]

    Pith/arXiv arXiv 2007

  36. [36]

    Winter, Photohadronic Origin of the TeV-PeV Neu- trinos Observed in IceCube, Phys

    W. Winter, Photohadronic Origin of the TeV-PeV Neu- trinos Observed in IceCube, Phys. Rev. D88, 083007 (2013), arXiv:1307.2793 [astro-ph.HE]

    Pith/arXiv arXiv 2013

  37. [37]

    Bustamante and I

    M. Bustamante and I. Tamborra, Using high-energy neutrinos as cosmic magnetometers, Phys. Rev. D102, 123008 (2020), arXiv:2009.01306 [astro-ph.HE]

    arXiv 2020

  38. [38]

    L. A. Anchordoqui, H. Goldberg, F. Halzen, and T. J. Weiler, Galactic point sources of TeV antineutrinos, Phys. Lett. B593, 42 (2004), arXiv:astro-ph/0311002

    Pith/arXiv arXiv 2004

  39. [39]

    Farzan, On theτflavor of the cosmic neutrino flux, JHEP07, 174, arXiv:2105.03272 [hep-ph]

    Y. Farzan, On theτflavor of the cosmic neutrino flux, JHEP07, 174, arXiv:2105.03272 [hep-ph]

    arXiv

  40. [40]

    Feldstein, A

    B. Feldstein, A. Kusenko, S. Matsumoto, and T. T. Yanagida, Neutrinos at IceCube from Heavy Decay- 32 ing Dark Matter, Phys. Rev. D88, 015004 (2013), arXiv:1303.7320 [hep-ph]

    Pith/arXiv arXiv 2013

  41. [41]

    Esmaili and P

    A. Esmaili and P. D. Serpico, Are IceCube neutrinos unveiling PeV-scale decaying dark matter?, JCAP11, 054, arXiv:1308.1105 [hep-ph]

    Pith/arXiv arXiv

  42. [42]

    Bhattacharya, M

    A. Bhattacharya, M. H. Reno, and I. Sarcevic, Reconcil- ing neutrino flux from heavy dark matter decay and re- cent events at IceCube, JHEP06, 110, arXiv:1403.1862 [hep-ph]

    Pith/arXiv arXiv

  43. [43]

    Barger and W.-Y

    V. Barger and W.-Y. Keung, Superheavy Particle Ori- gin of IceCube PeV Neutrino Events, Phys. Lett. B727, 190 (2013), arXiv:1305.6907 [hep-ph]

    Pith/arXiv arXiv 2013

  44. [44]

    C. A. Arg¨ uelles, K. Farrag, T. Katori, R. Khan- delwal, S. Mandalia, and J. Salvad´ o, Sterile neutri- nos in astrophysical neutrino flavor, JCAP02, 015, arXiv:1909.05341 [hep-ph]

    arXiv 1909

  45. [45]

    Ahlers, M

    M. Ahlers, M. Bustamante, and N. G. N. Willesen, Fla- vors of astrophysical neutrinos with active-sterile mix- ing, JCAP07, 029, arXiv:2009.01253 [hep-ph]

    arXiv 2009

  46. [46]

    O. Mena, I. Mocioiu, and S. Razzaque, Oscillation ef- fects on high-energy neutrino fluxes from astrophysi- cal hidden sources, Phys. Rev. D75, 063003 (2007), arXiv:astro-ph/0612325

    Pith/arXiv arXiv 2007

  47. [47]

    Razzaque and A

    S. Razzaque and A. Y. Smirnov, Flavor conversion of cosmic neutrinos from hidden jets, JHEP03, 031, arXiv:0912.4028 [hep-ph]

    Pith/arXiv arXiv

  48. [48]

    Sahu and B

    S. Sahu and B. Zhang, Effect of Resonant Neu- trino Oscillation on TeV Neutrino Flavor Ratio from Choked GRBs, Res. Astron. Astrophys.10, 943 (2010), arXiv:1007.4582 [hep-ph]

    Pith/arXiv arXiv 2010

  49. [49]

    Varela, S

    K. Varela, S. Sahu, A. F. Osorio Oliveros, and J. C. Sanabria, High energy neutrinos from choked GRBs and their flavor ratio measurement by the IceCube, Eur. Phys. J. C75, 289 (2015), arXiv:1411.7992 [astro- ph.HE]

    Pith/arXiv arXiv 2015

  50. [50]

    Xiao and Z

    D. Xiao and Z. G. Dai, TeV-PeV Neutrino Oscillation of Low-luminosity Gamma-ray Bursts, Astrophys. J.805, 137 (2015), arXiv:1504.01603 [astro-ph.HE]

    Pith/arXiv arXiv 2015

  51. [51]

    P. S. B. Dev, S. Jana, and Y. Porto, Matter effects on fla- vor composition of astrophysical neutrinos, Phys. Rev. D112, 093003 (2025), arXiv:2312.17315 [hep-ph]

    arXiv 2025

  52. [52]

    Q. Liu, D. F. G. Fiorillo, C. A. Arg¨ uelles, M. Busta- mante, N. Song, and A. C. Vincent, Identifying energy- dependent flavor transitions in high-energy astrophysi- cal neutrino measurements, Phys. Rev. D112, 043019 (2025), arXiv:2312.07649 [astro-ph.HE]

    arXiv 2025

  53. [53]

    Telalovic and M

    B. Telalovic and M. Bustamante, Flavor anisotropy in the high-energy astrophysical neutrino sky, JCAP05, 013, arXiv:2310.15224 [astro-ph.HE]

    arXiv

  54. [54]

    Telalovic and M

    B. Telalovic and M. Bustamante, No flavor anisotropy in the high-energy neutrino sky upholds Lorentz invari- ance, JHEP02, 024, arXiv:2503.15468 [hep-ph]

    arXiv

  55. [55]

    J. P. Rachen and P. M´ esz´ aros, Photohadronic neutrinos from transients in astrophysical sources, Phys. Rev. D 58, 123005 (1998), arXiv:astro-ph/9802280

    Pith/arXiv arXiv 1998

  56. [56]

    Athar, M

    H. Athar, M. Jezabek, and O. Yasuda, Effects of neu- trino mixing on high-energy cosmic neutrino flux, Phys. Rev. D62, 103007 (2000), arXiv:hep-ph/0005104

    Pith/arXiv arXiv 2000

  57. [57]

    R. M. Crocker, F. Melia, and R. R. Volkas, Searching for long wavelength neutrino oscillations in the distorted neutrino spectrum of galactic supernova remnants, Astrophys. J. Suppl.141, 147 (2002), arXiv:astro- ph/0106090

    arXiv 2002

  58. [58]

    Barenboim and C

    G. Barenboim and C. Quigg, Neutrino Observatories can Characterize Cosmic Sources and Neutrino Prop- erties, Phys. Rev. D67, 073024 (2003), arXiv:hep- ph/0301220

    arXiv 2003

  59. [59]

    J. F. Beacom, N. F. Bell, D. Hooper, S. Pakvasa, and T. J. Weiler, Measuring Flavor Ratios of High-Energy Astrophysical Neutrinos, Phys. Rev. D68, 093005 (2003), [Erratum: Phys. Rev. D 72, 019901 (2005)], arXiv:hep-ph/0307025

    Pith/arXiv arXiv 2003

  60. [60]

    J. F. Beacom and J. Candia, Shower power: Isolat- ing the prompt atmospheric neutrino flux using electron neutrinos, JCAP11, 009, arXiv:hep-ph/0409046

    Pith/arXiv arXiv

  61. [61]

    Kachelrieß and R

    M. Kachelrieß and R. Tom` as, High energy neutrino yields from astrophysical sources I: Weakly magnetized sources, Phys. Rev. D74, 063009 (2006), arXiv:astro- ph/0606406

    arXiv 2006

  62. [62]

    Esmaili and Y

    A. Esmaili and Y. Farzan, An Analysis of Cosmic Neu- trinos: Flavor Composition at Source and Neutrino Mixing Parameters, Nucl. Phys. B821, 197 (2009), arXiv:0905.0259 [hep-ph]

    Pith/arXiv arXiv 2009

  63. [63]

    Choubey and W

    S. Choubey and W. Rodejohann, Flavor Composition of UHE Neutrinos at Source and at Neutrino Telescopes, Phys. Rev. D80, 113006 (2009), arXiv:0909.1219 [hep- ph]

    Pith/arXiv arXiv 2009

  64. [64]

    H¨ ummer, M

    S. H¨ ummer, M. Maltoni, W. Winter, and C. Yaguna, Energy dependent neutrino flavor ratios from cosmic ac- celerators on the Hillas plot, Astropart. Phys.34, 205 (2010), arXiv:1007.0006 [astro-ph.HE]

    Pith/arXiv arXiv 2010

  65. [65]

    Palladino, G

    A. Palladino, G. Pagliaroli, F. L. Villante, and F. Vis- sani, What is the Flavor of the Cosmic Neutrinos Seen by IceCube?, Phys. Rev. Lett.114, 171101 (2015), arXiv:1502.02923 [astro-ph.HE]

    Pith/arXiv arXiv 2015

  66. [66]

    Bustamante, J

    M. Bustamante, J. F. Beacom, and W. Winter, The- oretically palatable flavor combinations of astrophys- ical neutrinos, Phys. Rev. Lett.115, 161302 (2015), arXiv:1506.02645 [astro-ph.HE]

    Pith/arXiv arXiv 2015

  67. [67]

    Biehl, A

    D. Biehl, A. Fedynitch, A. Palladino, T. J. Weiler, and W. Winter, Astrophysical Neutrino Production Diag- nostics with the Glashow Resonance, JCAP01, 033, arXiv:1611.07983 [astro-ph.HE]

    Pith/arXiv arXiv

  68. [68]

    Bustamante and M

    M. Bustamante and M. Ahlers, Inferring the flavor of high-energy astrophysical neutrinos at their sources, Phys. Rev. Lett.122, 241101 (2019), arXiv:1901.10087 [astro-ph.HE]

    Pith/arXiv arXiv 2019

  69. [69]

    Ackermannet al., Astrophysics Uniquely Enabled by Observations of High-Energy Cosmic Neutrinos, Bull

    M. Ackermannet al., Astrophysics Uniquely Enabled by Observations of High-Energy Cosmic Neutrinos, Bull. Am. Astron. Soc.51, 185 (2019), arXiv:1903.04334 [astro-ph.HE]

    Pith/arXiv arXiv 2019

  70. [70]

    Alves Batistaet al., EuCAPT White Paper: Op- portunities and Challenges for Theoretical Astroparticle Physics in the Next Decade, (2021), arXiv:2110.10074 [astro-ph.HE]

    R. Alves Batistaet al., EuCAPT White Paper: Op- portunities and Challenges for Theoretical Astroparticle Physics in the Next Decade, (2021), arXiv:2110.10074 [astro-ph.HE]

    arXiv 2021

  71. [71]

    Q. Liu, N. Song, and A. C. Vincent, Probing neu- trino production in high-energy astrophysical neutrino sources with the Glashow resonance, Phys. Rev. D108, 043022 (2023), arXiv:2304.06068 [astro-ph.HE]

    arXiv 2023

  72. [72]

    Bhattacharya, R

    A. Bhattacharya, R. Enberg, M. H. Reno, and I. Sarce- vic, Energy-dependent flavour ratios in neutrino tele- scopes from charm, JCAP03, 057, arXiv:2309.09139 [astro-ph.HE]

    arXiv

  73. [73]

    J. F. Beacom, N. F. Bell, D. Hooper, S. Pakvasa, and T. J. Weiler, Decay of High-Energy Astrophysical Neu- trinos, Phys. Rev. Lett.90, 181301 (2003), arXiv:hep- ph/0211305. 33

    arXiv 2003

  74. [74]

    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

    Pith/arXiv arXiv 2004

  75. [75]

    J. F. Beacom, N. F. Bell, D. Hooper, S. Pakvasa, and T. J. Weiler, Sensitivity toθ13 andδin the Decaying As- trophysical Neutrino Scenario, Phys. Rev. D69, 017303 (2004), arXiv:hep-ph/0309267

    Pith/arXiv arXiv 2004

  76. [76]

    P. D. Serpico, Probing the 2-3 leptonic mixing at high- energy neutrino telescopes, Phys. Rev. D73, 047301 (2006), arXiv:hep-ph/0511313

    Pith/arXiv arXiv 2006

  77. [77]

    Pakvasa, W

    S. Pakvasa, W. Rodejohann, and T. J. Weiler, Flavor Ratios of Astrophysical Neutrinos: Implications for Pre- cision Measurements, JHEP02, 005, arXiv:0711.4517 [hep-ph]

    Pith/arXiv arXiv

  78. [78]

    Esmaili, Pseudo-Dirac Neutrino Scenario: Cosmic Neutrinos at Neutrino Telescopes, Phys

    A. Esmaili, Pseudo-Dirac Neutrino Scenario: Cosmic Neutrinos at Neutrino Telescopes, Phys. Rev. D81, 013006 (2010), arXiv:0909.5410 [hep-ph]

    Pith/arXiv arXiv 2010

  79. [79]

    Bhattacharya, S

    A. Bhattacharya, S. Choubey, R. Gandhi, and A. Watanabe, Diffuse Ultra-High Energy Neutrino Fluxes and Physics Beyond the Standard Model, Phys. Lett. B690, 42 (2010), arXiv:0910.4396 [hep-ph]

    Pith/arXiv arXiv 2010

  80. [80]

    Bhattacharya, S

    A. Bhattacharya, S. Choubey, R. Gandhi, and A. Watanabe, Ultra-high neutrino fluxes as a probe for non-standard physics, JCAP09, 009, arXiv:1006.3082 [hep-ph]

    Pith/arXiv arXiv

Showing first 80 references.