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Bahcall, John N.; Lisi, E.; Alburger, D.E.; Braeckeleer, L. De; Freedman, S. J.; Napolitano, J.

doi:10.1103/physrevc.54.411

Cited by 189 publications

(279 citation statements)

References 53 publications

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“…If we make the imprecise approximations that are listed below, then we also do not find any allowed vacuum solutions at the 3σ CL. Here are the approximations (with references to descriptions of more accurate error treatments) : 1) neglect the uncertainty [45] in the true shape of the 8 B undistorted energy spectrum, 2) neglect the dependence on the neutrino oscillation parameters of the calculated errors for the SNO and Super-Kamiokande spectral energy distributions (i. e., compute the errors for an undistorted 8 B energy spectrum so that the percentage errors for each energy bin are independent of ∆m 2 and tan 2 θ ), and 3) neglect the correlations and energy dependence of the errors [5,47] for the chlorine and gallium neutrino cross sections. Making these approximations, we find that the ∆χ 2 between the best-fit LMA solution and the vacuum solution with the lowest χ 2 is 14.6 for the two-step SNO procedure and is 12.3 for the analysis including the full SNO day-night energy spectrum.…”

Section: Discussion and Summarymentioning

confidence: 99%

“…Table 6: Neutrino oscillation predictions for the chlorine and gallium radiochemical experiments. The predictions are based upon the global analysis strategy (a), and use the neutrino fluxes for the BP00 standard solar model (except for the 8 B flux for which the factor f B is included) and the neutrino absorption cross sections [49,45,47]. The rates are presented for the best-fit oscillation parameters of the allowed solutions listed in table 1.…”

Section: Discussion and Summarymentioning

confidence: 99%

See 1 more Smart Citation

Before and After: How has the SNO NC measurement changed things?

Bahcall¹,

González-García²,

Peña-Garay³

2002

J. High Energy Phys.

126

121

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We present "Before and After" global oscillation solutions, as well as predicted "Before and After" values and ranges for ten future solar neutrino observables (for BOREXINO, KamLAND, SNO, and a generic p − p neutrino detector). The "Before" case includes all solar neutrino data (and some theoretical improvements) available prior to April 20, 2002 and the "After" case includes, in addition, the new SNO data on the CC, NC, and day-night asymmetry. We have performed global analyses using the full SNO day-night energy spectrum and, alternatively, using just the SNO NC and CC rates and the day-night asymmetry. The LMA solution is the only currently allowed MSW oscillation solution at ∼ 99% CL. The LOW solution is allowed only at more than 2.5σ, SMA is now excluded at 3.7σ or 4.7σ depending upon analysis strategy, and pure sterile oscillations are excluded at more than 4.7σ. Small mixing angles are "out" (pure sterile is "way out"); MSW with large mixing angles is definitely "in." Vacuum oscillations are allowed at 3σ, but not at 2σ. Precise maximal mixing is excluded at 3.2σ for MSW solutions and at more than 2.8σ for vacuum solutions. Most of the predicted values for future observables for the BOREXINO, KamLAND, and future SNO measurements are changed only by minor amounts by the inclusion of the recent SNO data. In order to test the robustness of the allowed neutrino oscillation regions that are inferred from the measurements and the predicted values for future solar neutrino observables, we have carried out calculations using a variety of strategies for analyzing the SNO and other experimental data.

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Section: Discussion and Summarymentioning

confidence: 99%

Section: Discussion and Summarymentioning

confidence: 99%

Before and After: How has the SNO NC measurement changed things?

Bahcall¹,

González-García²,

Peña-Garay³

2002

J. High Energy Phys.

126

121

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show abstract

“…, 41, corresponding to the Super-Kamiokande energy bins) are divided in theoretical, (σ (th) cor ) j , and experimental systematic, (σ (sys) cor ) j . The theoretical correlated uncertainties (σ (th) cor ) j = R (th) j δ (th) j,cor come from the calculation of the shape of the 8 B energy spectrum [63,64]. We list in Table 4 the values of δ (th) j,cor that we have extracted from Fig.…”

Section: Global Analysismentioning

confidence: 99%

Bayesian view of solar neutrino oscillations

Garzelli

Giunti

2001

J. High Energy Phys.

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We present the results of a Bayesian analysis of solar neutrino data in terms of ν e → ν µ,τ and ν e → ν s oscillations, where ν s is a sterile neutrino. We perform a Rates Analysis of the rates of solar neutrino experiments, including the first SNO CC result, and spectral data of the CHOOZ experiment, and a Global Analysis that takes into account also the Super-Kamiokande day and night electron energy spectra. We show that the Bayesian analysis of solar neutrino data does not suffer any problem from the inclusion of the numerous bins of the CHOOZ and Super-Kamiokande electron energy spectra and allows to reach the same conclusions on the favored type of neutrino transitions and on the determination of the most favored values of the oscillation parameters in both the Rates and Global Analysis. Our Bayesian analysis shows that ν e → ν s transitions are strongly disfavored with respect to ν e → ν µ,τ transitions. In the case of ν e → ν µ,τ oscillations, the Large Mixing Angle region is favored by the data (86% probability), the LOW region has some small chance (13% probability), the Vacuum Oscillation region is almost excluded (1% probability) and the Small Mixing Angle region is practically excluded (0.01% probability). We calculate also the marginal posterior probability distributions for tan 2 ϑ and ∆m 2 in the case of ν e → ν µ,τ oscillations and we show that the data imply large mixing almost with certainty and large values of ∆m 2 are favored (2 × 10 −6 eV 2 < ∆m 2 < 10 −3 eV 2 with 86% probability). We present also the results of a standard least-squares analysis of solar neutrino data and we show that the standard goodness of fit test is not able to reject pure ν e → ν s transitions. The likelihood ratio test, which is insensitive to the number of bins of the CHOOZ and Super-Kamiokande energy spectra, allows to reject pure ν e → ν s transitions in favor of ν e → ν µ,τ transitions only in the Global Analysis.

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“…Those isotopes are chemically extracted and counted using their decay. The cross sections for 37 Cl(ν e ,e − ) 37 Ar [3] and 71 Ga(ν e ,e − ) 71 Ge [4] reactions, and the expected ν e energy spectrum from the 27 Al target are plotted in Fig. 2 (a).…”

Section: Radiochemical Detectorsmentioning

confidence: 99%

Neutrino Interactions with Matter by a New Neutrino Source From the Isotope Radioactive Decay Produced by the Proton Accelerator

Shin¹,

Park²,

Kajino³

et al. 2017

Proceedings of the 14th International Symposium on Nuclei in the Cosmos (NIC2016)

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A new neutrino source for future's neutrino experiments is suggested in this work. Unstable isotope, 27 Si, can be produced when 27 Al target is bombarded by 15 MeV proton beams. Through the decay of the 27 Si, a new electron-neutrino source in the 0 ∼ 5.0 MeV energy range is obtained. Production of the neutrino source is studied by using GEANT4 code with JENDL-4.0/HE. For radioactive decay processes, we use "G4RadioactiveDecay" model based on the Evaluated Nuclear Structure Data File (ENSDF). As for the detection system of the new neutrino source, we evaluate reaction or event rates for available radiochemical detectors and LENA type scintillator detector.

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Standard neutrino spectrum fromB8decay

Cited by 189 publications

References 53 publications

Before and After: How has the SNO NC measurement changed things?

Before and After: How has the SNO NC measurement changed things?

Bayesian view of solar neutrino oscillations

Neutrino Interactions with Matter by a New Neutrino Source From the Isotope Radioactive Decay Produced by the Proton Accelerator

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