Astrophysical neutrinos: flavor ratios depend on energy

Electromagnetic (and adiabatic) energy losses of pi's and mu's modify the flavor ratio (measured at Earth) of neutrinos produced by pi decay in astrophysical sources, Phi v: phi v mu: phi v 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 v energy, and is correlated with a modification of the neutrino spectrum. For gamma-ray bursts, e.g., the transition is expected at approximately 100 TeV and may be detected by km-scale v telescopes. Measurements of the transition energy and energy width will provide unique probes of the physics of the sources. Pi and mu energy losses also affect the ratio of ve flux to total v flux, which may be measured at the 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 p p (p gamma) interactions.