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See, for example, V. Berezinsky, Invited Lecture at 25th ICRC, Durban, 1997, astro-ph/9710126.
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Berezinsky, V.1
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12
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85038885375
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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 (Formula presented) 67, or that (Formula presented) 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 (Formula presented) in this case, a positive signal for the CHOOZ experiment 9; therefore both scenarios are currently not supported by the data
-
There have been several attempts to reconcile all detected anomalies with a scheme involving only three neutrino flavors, suggesting for example that (Formula presented) 67, or that (Formula presented) 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 (Formula presented) 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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14
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17
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85038920619
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The current value for the number of standard light neutrinos is (Formula presented) see LEP Electroweak Working Group, CERN/PPE/95–172
-
The current value for the number of standard light neutrinos is (Formula presented) see LEP Electroweak Working Group, CERN/PPE/95–172.
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18
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0542394553
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85038928073
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The enhancement of the amplitude of oscillations at (Formula presented) in the case of (Formula presented) mixing, can be understood 16 as a case of “parametric resonance” 25
-
The enhancement of the amplitude of oscillations at (Formula presented) in the case of (Formula presented) mixing, can be understood 16 as a case of “parametric resonance” 25.
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44
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85038927745
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-
The dashed curves in Figs. 33 and 44 are calculated assuming a constant density in the core and mantle of the earth (Formula presented) and (Formula presented) calculated averaging the density along a trajectory of zenith angle (Formula presented)
-
The dashed curves in Figs. 33 and 44 are calculated assuming a constant density in the core and mantle of the earth (Formula presented) and (Formula presented) calculated averaging the density along a trajectory of zenith angle (Formula presented)
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45
-
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85038911682
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Note in the lower panels of Figs. 55 and 66 that the suppression factor for (Formula presented) 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. 33
-
Note in the lower panels of Figs. 55 and 66 that the suppression factor for (Formula presented) 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. 33.
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46
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0001041162
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48
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85038967665
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We note that in 17 the authors have considered only the case of positive (Formula presented) Matter effects allow to distinguish the case of positive and negative squared mass differences, and the allowed region for (Formula presented) is somewhat larger than in the other case, because of the MSW resonance present for the neutrinos
-
We note that in 17 the authors have considered only the case of positive (Formula presented) Matter effects allow to distinguish the case of positive and negative squared mass differences, and the allowed region for (Formula presented) is somewhat larger than in the other case, because of the MSW resonance present for the neutrinos.
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52
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85038893503
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The flux of (Formula presented)-induced muons is larger than the flux of atmospheric muons for line of sights shielded by a column density larger than (Formula presented) In the upper hemisphere this condition is satisfied at most in a small solid angle for the deepest detectors
-
The flux of (Formula presented)-induced muons is larger than the flux of atmospheric muons for line of sights shielded by a column density larger than (Formula presented) In the upper hemisphere this condition is satisfied at most in a small solid angle for the deepest detectors.
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54
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85038943251
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Kamiokande Collaboration, A. Suzuki et al., in Proceedings of 7th International Workshop on Neutrino Telescopes, Venice, 1996, edited by M. Baldo Ceolin, p. 263.
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85038966495
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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
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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.
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