Analysis of Neutrino Oscillation in Three-Flavor Neutrinos

Sakai, Toyokazu; Inagaki, O.; Teshima, Tadayuki

doi:10.1142/s0217751x99000981

Cited by 16 publications

(3 citation statements)

References 32 publications

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“…set by the CHOOZ [19] long baseline reactor in the disappearance mode ν e → ν x , an analysis in Ref. [6] also has given allowed ranges of δ 2 and sin 2 2θ for φ < 20 • . Note that to zeroth order of δ 2 /∆ 2 , the probability becomes [18] P (ν e → ν e ) ≃ cos 4 φP 2ν + sin 4 φ.…”

Section: A Sn Neutrinos and Neutrino Parametersmentioning

confidence: 99%

“…The flavor oscillation can be parameterized by the mass-squared differences of the neutrino mass eigenstates ∆m 2 ≡ m 2 i − m 2 j (i, j = 1, 2, 3) and θ ij , the mixing angles between weak eigenstates and mass eigenstates of the neutrinos (θ ij ≤ π 4 is assumed). In terms of these parameters, the just-so vacuum oscillation [4] requires 6 × 10 −11 ≤ ∆m 2 ≤ 60 × 10 −11 eV 2 and sin 2 2θ ≃ 1, while the MSW resonant effect [5] in the Sun becomes important if 4 × 10 −6 eV 2 ≤ ∆m 2 ≤ 7 × 10 −5 eV 2 , sin 2 2θ ≃ 0.6 − 0.9 (large angle solution), or 3 × 10 −6 eV 2 ≤ ∆m 2 ≤ 12 × 10 −6 eV 2 , 0.003 ≤ sin 2 2θ ≤ 0.01 (small angle solution) [6]. Recent atmospheric neutrino data from the Super-Kamiokande [7] further provide a strong evidence in support of neutrino oscillation as the cause to deficit of muon neutrinos, provided ∆m 2 ∼ 10 −2 − 10 −3 eV 2 and sin 2 2θ > 0.82.…”

Section: Introductionmentioning

confidence: 99%

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Effects of neutrino temperatures and mass hierarchies on the detection of supernova neutrinos

Chiu

Kuo

2000

Phys. Rev. D

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Possible outcomes of neutrino events at both Super-Kamiokande and SNO for a type-II supernova are analyzed considering the uncertainties in SN neutrino spectra (temperature) at emission, which may complicate the interpretation of the observed events. With the input of parameters deduced from the current solar and atmospheric experiments, consequences of direct-mass hierarchy m ντ ≫ m νµ > m νe and inverted-mass hierarchy m νe > m νµ ≫ m ντ are investigated. Even if the ν temperatures are not precisely known, we found that future experiments are likely to be able to separate the currently accepted solutions to the solar neutrino problem (SNP): large angle MSW, small angle MSW, and the vacuum oscillation, as well as to distinguish between the direct and inverted mass hierarchies of the neutrinos.

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Section: A Sn Neutrinos and Neutrino Parametersmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Effects of neutrino temperatures and mass hierarchies on the detection of supernova neutrinos

Chiu

Kuo

2000

Phys. Rev. D

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“…There have been many analytic works on three-flavor MSW solutions of the solar neutrino problem with simple linear and exponential matter densities [33][34][35][36][37][38][39][40]. Most three-flavor MSW fits to the solar neutrino experiments have been made within the above framework [41][42][43][44][45]. Recently exact solutions to the three neutrino MSW equations for such simple matter densities were derived [46][47][48].…”

Section: Introductionmentioning

confidence: 99%

The earth regeneration effect of solar neutrinos: a numerical treatment with three active neutrino flavors

Kim

Lee

2001

Computer Physics Communications

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We introduce an integrated algorithm for full scale investigation of the earth regeneration effect of solar neutrinos with all three active neutrinos. We illustrate that the earth effect on low energy solar neutrinos (Eν < 20 MeV) causes large variations in the survival probabilities for large values of the mixing angle θ12 for a given value of θ13. But it is maximal for small values of θ13 and diminishes for large values at a given value of θ12. The nadir angle dependence is sensitive to the value of E ′ ≡ E/∆12. As far as low energy solar neutrinos are concerned we notice that the earth effect is more pronounced for core penetration. We confirm that the earth effect leaves the SMA region almost intact regardless of θ13 and that it is significant for high energy 8 B and hep neutrinos in the LMA region. We also show that for large values of θ13, the earth effect is significant for high energy neutrinos (E ′ > ∼ 10 9 ) and it can be large at any nadir angle.PACS numbers: 14.60.Pq; 26.65.+t; 96.60.Jw I. INTRODUCTIONNeutrinos are produced abundantly from thermonuclear reactions taking place in the stellar core. They carry away most of the energy during the supernova explosion. Due to the extreme weakness of its interaction it escapes its cradle almost intact and provides us with most reliable clues to the internal physical environments of a star. Thus neutrino astronomy has been established as an important research field recently. The Standard Solar model (SSM) [1-3] predicts the flux of the electron neutrino. The historic Homestake experiment [4] for detecting solar neutrinos revealed that the detected neutrinos fall far short of the SSM prediction.Several mechanisms were proposed for the depletion of solar neutrinos. Pontecorvo [5] proposed the idea of neutrino flavor oscillation earlier than any unification theories [6]. (see ref.[7] for an interesting review). The possibility of solar neutrino flux reduction by vacuum oscillation was investigated earlier [8,9]. Subsequent experiments [10][11][12][13] revealed that the solar neutrino deficit depends on the energy of the neutrino. Recently the idea of flavor oscillation combined with the Mikheyev-Smirnov-Wolfenstein (MSW) effect [14,15] has been most popular. The MSW equations have been vigorously studied. For simple matter densities, some authors [16-20] derived accurate analytic solutions for the two-neutrino MSW evolution equations. These solutions have been used for computing the neutrino survival probabilities with the approximation of the solar matter density by a mosaic of exponential functions. Direct numerical analysis was carried out also [21]. Two-flavor MSW solutions to the solar neutrino puzzle were fully analysed with high accuracy, including both the day/night effect and spectral information [22,23].Recent Super-Kamiokande experiment [24] shows an evidence for oscillations of the atmospheric neutrinos [25][26][27][28]. The data are in good agreement with two-flavor ν µ ↔ ν τ oscillations. These results did establish that neutrinos oscillate and poss...

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Atmospheric neutrinos: LMA oscillations, Ue3 induced interference and CP-violation

2004

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Analysis of Neutrino Oscillation in Three-Flavor Neutrinos

Abstract: We analyzed the solar, terrestrial and atmospheric neutrinos experiments using the three-flavor neutrino framework and got the allowed regions for param- is favored than the small angle slution from the analysis of zenith angle dependence in atmospheric neutrino sub-GeV experiment.

Cited by 16 publications

References 32 publications

Effects of neutrino temperatures and mass hierarchies on the detection of supernova neutrinos

Effects of neutrino temperatures and mass hierarchies on the detection of supernova neutrinos

The earth regeneration effect of solar neutrinos: a numerical treatment with three active neutrino flavors

Atmospheric neutrinos: LMA oscillations, Ue3 induced interference and CP-violation

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