Neutrino oscillation

The discrepancies in both Tables V and VI probably stem from neutrino oscillations. Briefly, the idea originated in the speculation that the energy eigenstates of the three known neutrinos might differ from the weak eigenstates of the neutrinos, Vg, and, that are found in the labora- 

Becker-Szendy Close to Kamiokande value for same  

Correspondingly, the probability that a beam initially of Vg remains Vg after traversing a distance L is 

The results from the astroneutrino experiments in Tables V and VI are consistent with different numerical descriptions of neutrino oscillations. One finds solutions in which Am is of the order of 10 eV from two MSW solutions and 10 eV from the so-called solar neutrino vacuum oscillation solution, nominally representing a Ve -o- oscillation. A fourth solution yields 10 eV  

There is reason to believe that the above properties reflect the major neutrino oscillation channels, although only one of the three solar neutrino solutions will ultimately turn out to be valid. Neutrino searches for oscillations at nuclear reactors in France, in southern California in the United States, and in Japan, all past or near the data-taking stage, will ultimately help clarify the choice of solutions. More importantly, at least one of those experiments or the experiments discussed below may provide a conclusive demonstration that the astroneutrino data is correctly interpreted by the neutrino oscillation explanation. 

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MARE [32-38], Neutrino oscillation experiments have proved that neutrinos are massive particles, but cannot determine their absolute mass scale. Therefore, the neutrino mass is still an open question in elementary particle physics. An international collaboration is growing around the project of microcalorimeter arrays for a rhenium experiment (MARE) for directly measuring the neutrino mass with a sensitivity of about 0.2eV/c1 2 4. 

In the last decade, neutrino experiments have demonstrated that neutrinos are massive particles which may oscillate among three autostates. Such experiments [77-82] have evidenced the mass difference between the autostates, but not the neutrino mass scale value. The only way to determine the neutrino mass is the knowledge of the shape of the end point of energy spectrum in beta decays. In the hypothesis of the Majorana neutrino (neutrino coincides with antineutrino and its rest mass is different from zero), the measure of the decay half-life in the neutrinoless double-beta decay (DBD) would be necessary. A number of recent theoretical interpretations of neutrino oscillation experiments data imply that the effective Majorana mass of the electron neutrino (as measured in neutrinoless DBD) could be in the range 0.01 eV to the present bounds. 

Super-Kamiokande light-water experiment reveals atmospheric neutrino oscillations. 

Neutrino oscillations in the weak matter effect regime have been discussed extensively before [1-13], in particular, for the solar and supemovae neutrinos propagating in the matter of the Earth. The previous work has been done mainly in the approximation of constant density profile which consists of several layers with constant density. 

The probability of u2 —> u, transition relevant for the solar neutrino oscillations in the Earth can be obtained immediately from the unitarily condition ... 

The solution to the solar neutrino problem is that something is wrong with our ideas of the fundamental structure of matter, the so-called standard model. This difficulty takes the form of neutrino oscillations as the solution to the solar neutrino... 

The direct observational evidence for the occurrence of neutrino oscillations came from observations with the Cerenkov detectors. The SNO detector found one-third the expected number of electron neutrinos coming from the sun in agreement with previous work with the radiochemical detectors. The Super Kamiokande detector, which is primarily sensitive to electron neutrinos, but has some sensitivity to other neutrino types found about one-half the neutrino flux predicted by the standard... 

Neutrino oscillations have up to now been detected in two systems. Atmospheric muon neutrinos, which originate from the collision of cosmic rays... 

The existence of such conversions, i.e., neutrino oscillations, cannot be considered completely proved at present. 

Although I will not discuss the subject here, The most important secondary cosmic-ray flux is the atmospheric neutrino beam because of the discovery of neutrino oscillations by Super-Kamiokande (Fukuda el al., 1998). The experimental situation is reviewed by Kajita Totsuka, 2001 and Jung el al., 2001, and the calculations by Gaisser Honda, 2002. 

For a long time the necessity to extend the Standard model had purely theoretical reasons. Aesthetically, because full unification is not achieved in the Standard model practically, because it contains some internal inconsistencies. It does not seem complete for cosmology. One has to go beyond the Standard model to explain inflation, baryosynthesis and nonbaryonic dark matter. Recently there has appeared a set of experimental evidences for the existence of neutrino oscillations (see review in [3]), of cosmic WIMPs [4], and of double neutrinoless beta decay [5]. Whatever is the accepted status of these evidences,... 

The search for rare processes, such as proton decay, neutrino oscillations, neutrinoless beta decay, precise measurements of parameters of known particles, experimental searches for dark matter represent the widely known forms of such means. 

Figure 7. Projected sensitivity using 149 GRB as a function of E M. Detector sensitivity (solid curves) are compared to Waxman-Bahcall (Waxman, 2003) (rescaled for neutrino oscillation) and precursor (Razzaque and Meszaros, 2003, Raz-zaque et al., 2003) model spectra.

G. G. Raffelt, M. Th. Keil, R. Buras, H.-Th. Janka, M. Rampp, astro-ph/0303226 Proc. 4th Workshop on Neutrino Oscillations and their Origin NOON (2003)... 

Nuclear neutrino research includes neutrino experiments such as SNO, Super-Kamiokande, KamLAND, SAGE, and double-beta decay and theory of neutrino oscillations. 

Derived from an analysis of neutrino-oscillation experiments. 

Detector parameters are taken from F. Suekane, Status of the KamLAND Experiment , Talk presented at Europhysics Neutrino Oscillation Workshop, (Now 98) 7-9 September 1998, Amsterdam, the Netherlands. 

W boson. This is interpreted as a signature that the weak interaction mixes the quark states. It is sufficient to assume that either the upper or the lower quark states are mixed. The lower quark states are taken to be mixed, and that is indicated by the apostrophes in O Table 10.1 on the symbols of the lower quarks. There is experimental evidence, neutrino oscillations, for the neutrinos also having a tiny little mass (Fukuda and et al. 1998) then of course the lepton states will be mixed as well for the weak interaction (Maid et al. 1962). 

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