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There have been several attempts to reconcile all detected anomalies with a scheme involving only three neutrino flavors, suggesting for example that Am SWD=Am ,m [6,7], or that AHiQ=A; ; i ,m [8]. The first scenario predicts the absence of a zenith angle dependence of the atmospheric neutrino anomaly, the second one predicts a constant suppression for all solar neutrino experiments and, since the atmospheric neutrino anomaly is essentially due to v/i< -> ve in this case, a positive signal for the CHOOZ experiment [9]; therefore both scenarios are currently not supported by the data.
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There have been several attempts to reconcile all detected anomalies with a scheme involving only three neutrino flavors, suggesting for example that Am SWD=Am ,m [6,7], or that AHiQ=A; ; i ,m [8]. The first scenario predicts the absence of a zenith angle dependence of the atmospheric neutrino anomaly, the second one predicts a constant suppression for all solar neutrino experiments and, since the atmospheric neutrino anomaly is essentially due to v/i< -> ve in this case, a positive signal for the CHOOZ experiment [9]; therefore both scenarios are currently not supported by the data.
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The dashed curves in Figs. 3 and 4 are calculated assuming a constant density in the core and mantle of the earth (pc(0z)) and (pm(0z)), calculated averaging the density along a trajectory of zenith angle 0Z.
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The dashed curves in Figs. 3 and 4 are calculated assuming a constant density in the core and mantle of the earth (pc(0z)) and (pm(0z)), calculated averaging the density along a trajectory of zenith angle 0Z.
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Note in the lower panels of Figs. 5 and 6 that the suppression factor for v -> v, transitions, if studied in great detail shows a complex dependence on the zenith angle that can be compared with the oscillation probability curves in Fig. 3.
-
Note in the lower panels of Figs. 5 and 6 that the suppression factor for v -> v, transitions, if studied in great detail shows a complex dependence on the zenith angle that can be compared with the oscillation probability curves in Fig. 3.
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We note that in [17] the authors have considered only the case of positive Am2. Matter effects allow to distinguish the case of positive and negative squared mass differences, and the allowed region for Aw2< 0 is somewhat larger than in the other case, because of the MSW resonance present for the neutrinos.
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The flux of r-induced muons is larger than the flux of atmospheric muons for line of sights shielded by a column density larger than ~ 106 g cm~2. In the upper hemisphere this condition is satisfied at most in a small solid angle for the deepest detectors.
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The flux of r-induced muons is larger than the flux of atmospheric muons for line of sights shielded by a column density larger than ~ 106 g cm~2. In the upper hemisphere this condition is satisfied at most in a small solid angle for the deepest detectors.
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The acceptance for the muon flux increases with the area (as opposed to the volume) of the detector: SK does not dominate the other experiments as for the contained neutrino events.
-
The acceptance for the muon flux increases with the area (as opposed to the volume) of the detector: SK does not dominate the other experiments as for the contained neutrino events.
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