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Astrophysical bounds on the high-energy evolution of neutrino mixing

Mauricio Bustamante1,*, Qinrui Liu2,3,†, and Gabriela Barenboim4,‡

  • *Contact author: mbustamante@nbi.ku.dk
  • †Contact author: qinrui_liu@sfu.ca
  • ‡Contact author: gabriela.barenboim@uv.es
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Phys. Rev. D 114, 055057 – Published 30 September, 2026

DOI: https://doi.org/10.1103/gvgb-x2pr

Abstract

While conventional oscillation experiments measure neutrino mixing parameters with high precision, these measurements are strictly confined to sub-TeV scales. At higher energies, renormalization-group effects can cause these parameters to evolve with the transferred momentum, Q. High-energy and ultra-high-energy astrophysical neutrinos, spanning TeV to EeV energies, probe high values of Q unreachable by conventional experiments, offering an unprecedented test of high-energy mixing. We use the flavor composition of these neutrinos—the relative proportions of νe, νμ, and ντ—to constrain this evolution, both phenomenologically and within dimension-6 Standard Model effective field theory. We account for astrophysical uncertainties—an unavoidable requirement to obtain realistic results, even though this weakens the bounds. Although present IceCube measurements lack the sensitivity to detect this running, we forecast that upcoming multidetector combinations will place unprecedented bounds on the high-energy evolution of neutrino mixing.

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Phys. Rev. D 114, 055057– Published 30 September, 2026
  • Received 3 May 2026
  • Accepted 2 September 2026
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