Conflict between the identification of cosmic neutrino source and the sensitivity to mixing angles in neutrino telescope

We suggest that neutrino fluxes to be measured at telescopes(the fluxes) can update somewhat of the contents in mass parameters due to the wide coverage of neutrino energy, which oscillation probabilities are less effective for. Two types of cosmic neutrinos are considered: one from pion source and the other from muon-damped source. The eightfold degeneracy is generated because oscillation probabilities are blind to (i) the sign of

\theta_{23}-\pi/4

, (ii) different pairs of

(\theta_{13},\delta)

and (iii) the sign of

\Delta m_{31}^2

. When the LBL oscillation in JHF constrains the fluxes, the

\Delta m_{31}^2

hidden in fluxes is exposed, so that the eightfold degeneracy is fully analyzed. The fluxes significantly sensitive to

\theta_{23}

without causing a degeneracy can improve the accuracy. The

\delta

curves of NH and IH for a given

\theta_{13}

in oscillation probability vs. the fluxes are so different from each other that

\Delta m_{31}^2

will be determined at once from

\theta_{13}

. Figures with different sources and with different fluxes include eight curves in each, one of which is the physical solution. By matching

(\theta_{13},\delta)

pairs, it is possible to determine the physical values of the pair, as well as those of

\theta_{23}

and

\Delta m_{31}^2

.

Note:

17 pages with 7 figures

14.60.Pq
98.70.Sa
95.55.Vj
neutrino: cosmic radiation
cosmic radiation: flux
neutrino: energy
neutrino: oscillation
cosmic radiation: particle source
neutrino: mixing angle
neutrino: mass difference

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