Ambiguity in source flux of cosmic/astrophysical neutrinos: Effects of bi-maximal mixing and quantum-gravity induced decoherence

For high energy cosmic neutrinos Athar, Jezabek, and Yasuda (AJY) have recently shown that the existing data on neutrino oscillations suggest that cosmic neutrino flux at the AGN/GRB source, F(nu (e)) : F(nu (mu)) : F(nu (tau)) approximate to 1 : 2 : 0, oscillates to F(nu (e)) : F(nu (e)) : F(nu (tau)) approximate to 1 : 1 : 1. These results can be confirmed at AMANDA, Baikal, ANTARES and NESTOR, and other neutrino detectors with a good flavor resolution. Here, we rederive the AJY result from quasi bi-maximal mixing, and show that observation of F(nu (e)) : F(nu (mu)) : F(nu (tau)) approximate to 1 : 1 : 1 does not necessarily establish cosmic neutrino flux at the AGN/GRB source to be F(v,) : F(nu (mu)) : F(nu (tau)) 1 : 2 : 0. We also note that if the length scale for the quantum-gravity induced decoherence for astrophysical neutrinos is of the order of a Mpc, then independent of the MNS matrix, the Liu-Hu-Ge (LHG) mechanism would lead to flux equalization for the cosmic/astrophysical neutrinos.