Four-neutrino oscillation solutions of the atmospheric neutrino anomaly

Fogli, G. L.; Lisi, E.; Marrone, A.

doi:10.1103/physrevd.63.053008

Cited by 66 publications

(74 citation statements)

References 44 publications

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“…In any case, mixed (active+sterile) solar neutrino oscillations are certainly still allowed [30], and can also be made consistent with the atmospheric neutrino oscillation evidence [31]. In the general case of active+sterile oscillations, Eqs.…”

Section: B Sterile Neutrino Oscillationssupporting

confidence: 51%

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Solar neutrino event spectra: Tuning SNO to equalize Super-Kamiokande

Fogli

Lisi²,

Palazzo³

et al. 2001

Phys. Rev. D

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The Super-Kamiokande (SK) and the Sudbury Neutrino Observatory (SNO) experiments are monitoring the flux of 8 B solar neutrinos through the electron energy spectrum from the reactions ν e,µ,τ + e − → ν e,µ,τ + e − and ν e + d → p + p+e − , respectively. We show that the SK detector response to 8 B neutrinos in each bin of the electron energy spectrum (above 8 MeV) can be approximated, with good accuracy, by the SNO detector response in an appropriate electron energy range (above 5.1 MeV). For instance, the SK response in the bin [10, 10.5] MeV is reproduced ("equalized") within ∼ 2% by the SNO response in the range [7.1, 11.75] MeV. As a consequence, in the presence of active neutrino oscillations, the SK and SNO event rates in the corresponding energy ranges turn out to be linearly related, for any functional form of the oscillation probability. Such equalization is not spoiled by the possible contribution of hep neutrinos (within current phenomenological limits). In perspective, when the SK and the SNO spectra will both be measured with high accuracy, the SK-SNO equalization can be used to determine the absolute 8 B neutrino flux, and to cross-check the (non)observation of spectral deviations in SK and SNO. At present, as an exercise, we use the equalization to "predict" the SNO energy spectrum, on the basis of the current SK data. Finally, we briefly discuss some modifications or limitations of our results in the case of sterile ν oscillations and of relatively large Earth matter effects. PACS number(s): 26.65.+t, 13.15.+g, 14.60.Pq

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Section: B Sterile Neutrino Oscillationssupporting

confidence: 51%

“…Since such ratios are small, the combined response functions ρ X [Eq. (31)] are always dominated by the ρ X B component, even for a relatively large hep flux (e.g., f hep /f B = 3). Therefore, we expect that, although the SK and SNO response functions to hep neutrinos can be noticeably different (see Fig.…”

Section: C)mentioning

confidence: 99%

Solar neutrino event spectra: Tuning SNO to equalize Super-Kamiokande

Fogli

Lisi²,

Palazzo³

et al. 2001

Phys. Rev. D

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“…This shows again (as does the recent illustrative study in Ref. [18]), that it would be valuable to carry out a more complete analysis of the SuperK and other atmospheric neutrino data with not just three-flavor oscillations, but also two ∆m 2 values included. Although the SuperK fit to its data shows that the ν µ ↔ ν e oscillations make a small contribution, it is important to include this contribution correctly, and the one-∆m 2 approximation is not, in general, reliable for this transition.…”

Section: Matter Effects For Neutrino Oscillations With Two Relevmentioning

confidence: 99%

“…One salient result is that in Ref. [18], the usual fit to the SuperK atmospheric neutrino data with a single ∆m 2 atm ≃ 3 × 10 −3 eV 2 and sin 2 (2θ atm ) = 1 is compared with a very different fit with two equal mass squared differences, ∆m 2 32 = ∆m 2 21 = 0.7 × 10 −3 eV 2 , and it is argued that although the χ 2 for the latter is worse, it is still an acceptable fit. This suggests that one should carefully assess corrections to the one-∆m 2 approximation in studies of neutrino oscillations.…”

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confidence: 99%

Neutrino Oscillations with Two Δm² Scales

Mocioiu

Shrock

2001

J. High Energy Phys.

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An approximation that is often used in fits to reactor and atmospheric neutrino data and in some studies of future neutrino oscillation experiments is to assume one dominant scale, ∆m 2 , of neutrino mass squared differences, in particular, ∆m 2 atm ∼ 3 × 10 −3 eV 2 . Here we investigate the corrections to this approximation arising from the quantity ∆m 2 sol relevant for solar neutrino oscillations, assuming the large mixing angle solution. We show that for values of sin 2 (2θ 13 ) ∼ 10 −2 (in the range of interest for long-baseline neutrino oscillation experiments with either intense conventional neutrino beams such as JHF-SuperK or a possible future neutrino factory) and for ∆m 2 sol ∼ 10 −4 eV 2 , the contributions to ν µ → ν e oscillations from both CP-conserving and CP-violating terms involving sin 2 (∆m 2 sol L/(4E)) can be comparable to the terms involving sin 2 (∆m 2 atm L/(4E)) retained in the one-∆m 2 approximation. Accordingly, we emphasize the importance of performing a full three-flavor, two-∆m 2 analysis of the data on ν µ → ν e oscillations in a conventional-beam experiment and ν e → ν µ ,ν e →ν µ oscillations at a neutrino factory. We also discuss a generalized analysis method for the KamLAND reactor experiment, and note how the information from this experiment can be used to facilitate the analysis of the subsequent data on ν µ → ν e oscillations. Finally, we consider the analysis of atmospheric neutrino data and present calculations of matter effects in a three-flavor, two-∆m 2 framework relevant to this data and to neutrino factory measurements. *

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“…Extensions of the Standard Model (SM) and/or new symmetries, e.g., horizontal symmetries, have been discussed thoroughly in connection with neutrino oscillation data [6,7,8,9,10,11]. A possibility to explain neutrino data through non-universal gauge interactions in the electroweak sector was discussed in Ref.…”

Section: Introductionmentioning

confidence: 99%

Neutrino oscillations due to nonuniversal gauge interactions in the weak sector

Malkawi

2002

Phys. Rev. D

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We discuss the structure of the neutrino mass matrix as derived from a nonuniversal electroweak gauge interaction model. We discuss two interesting patterns of neutrino masses. The first pattern is hierarchal which fits the LMA or LOW solutions of solar neutrino data. The second pattern gives rise to inverted mass spectrum which fits the currently not preferred SMA solution. The mechanism for generating a light sterile neutrino mass is interesting and is briefly discussed.

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Four-neutrino oscillation solutions of the atmospheric neutrino anomaly

Cited by 66 publications

References 44 publications

Solar neutrino event spectra: Tuning SNO to equalize Super-Kamiokande

Solar neutrino event spectra: Tuning SNO to equalize Super-Kamiokande

Neutrino Oscillations with Two Δm² Scales

Neutrino oscillations due to nonuniversal gauge interactions in the weak sector

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Four-neutrino oscillation solutions of the atmospheric neutrino anomaly

Cited by 66 publications

References 44 publications

Solar neutrino event spectra: Tuning SNO to equalize Super-Kamiokande

Solar neutrino event spectra: Tuning SNO to equalize Super-Kamiokande

Neutrino Oscillations with Two Δm2 Scales

Neutrino oscillations due to nonuniversal gauge interactions in the weak sector

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Product

Resources

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Neutrino Oscillations with Two Δm² Scales