Flavoring Astrophysical Neutrinos: Flavor Ratios Depend on Energy
read the original abstract
Electromagnetic (and adiabatic) energy losses of pions and muons modify the flavor ratio (measured at Earth) of neutrinos produced by pion decay in astrophysical sources, $\Phi_{\nu_e}:\Phi_{\nu_\mu}:\Phi_{\nu_\tau}$, from 1:1:1 at low energy to 1:1.8:1.8 at high energy. The transition occurs over 1-2 decades of nuetrino energy, and is correlated with a modification of the neutrino spectrum. For gamma-ray bursts, e.g., the transition is expected at \~100 TeV, and may be detected by km-scale neutrino telescopes. Measurements of the transition energy and energy-width will provide unique probes of the physics of the sources. pion and muon energy losses also affect the ratio of $\bar\nu_e$ flux to total neutrino flux, which may be measured at the W-resonance (6.3 PeV): It is modified from 1/6 (1/15) at low energy to 1/9 (practically 0) at high energy for neutrinos produced in pp ($p\gamma$) interactions.
This paper has not been read by Pith yet.
Forward citations
Cited by 3 Pith papers
-
Little Red Dots as Hidden Neutrino Sources
Little Red Dots can contribute ~30% of the diffuse neutrino background at TeV-sub-PeV energies through photomeson production in black hole envelopes, with modified flavor ratios at higher energies.
-
Ultra-High-Energy Tau Neutrinos as Probes of Lorentz Invariance
Ultra-high-energy tau neutrino detections at GRAND and POEMMA are projected to constrain Lorentz invariance violation parameters orders of magnitude more stringently than current lower-energy probes.
-
Astrophysical bounds on the high-energy evolution of neutrino mixing
High-energy astrophysical neutrinos can constrain the running of neutrino mixing parameters with energy, with future multi-detector setups forecast to set strong bounds despite astrophysical uncertainties.
discussion (0)
Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.