Gallium solar neutrino experiments: Absorption cross sections, neutrino spectra, and predicted event rates

Bahcall, John N.

doi:10.1103/physrevc.56.3391

Cited by 234 publications

(326 citation statements)

References 55 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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“…Using the 1998 standard value S 17 (0) = 19 +4 −2 eVb [19], the 8 B neutrino flux was calculated previously to be φ 8 B = 5.05 1.00 +0. 20 −0.16 . The total rates were calculated using the neutrino absorption cross sections and their uncertainties that are given in ref.…”

Section: Fluxesmentioning

confidence: 99%

“…The total rates were calculated using the neutrino absorption cross sections and their uncertainties that are given in ref. [20] element diffusion coefficients. In addition, the 14 N + p reaction causes a 0.2% uncertainty in the predicted pp flux, a 0.1 SNU uncertainty in the Cl event rate, and a 1 SNU uncertainty in the Ga event rate.…”

Section: Fluxesmentioning

confidence: 99%

Robust signatures of solar neutrino oscillation solutions

Bahcall

González-García

Peña-Garay

2002

J. High Energy Phys.

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With the goal of identifying signatures that select specific neutrino oscillation parameters, we test the robustness of global oscillation solutions that fit all the available solar and reactor experimental data. We use three global analysis strategies previously applied by different authors and also determine the sensitivity of the oscillation solutions to the critical nuclear fusion cross section, S 17 (0), for the production of 8 B. Our standard results make use of the precise new measurement of S 17 (0) by Junghans et al. The globally favored solutions are, in order of goodness of fit: LMA(the only solution at 2σ), LOW, and VAC. The NC to CC ratio for SNO is predicted by the standard global analysis to be 3.45 +0.70 −0.54 (1σ) which is separated from the no-oscillation value of 1.0 by much more than the expected experimental error. The predicted range of the day-night difference in CC rates is 8.3 +5.0 −5.6 (1σ)%. A measurement by SNO of either a NC to CC ratio > 3.3 or a day-night difference > 10%, would favor a small region of the currently allowed LMA neutrino parameter space. The global oscillation solution predicts a 7 Be neutrino-electron scattering rate in BOREXINO and KamLAND in the range 0.65 +0.04 −0.03 (1σ) of the BP00 standard solar model rate, a prediction which can be used to test both the solar model and the neutrino oscillation theory. Only the LOW solution predicts a large day-night effect(≤ 42%, 3σ) in BOREXINO and KamLAND. For the reactor KamLAND experiment, the LMA solution predicts a charged current rate relative to the standard model of 0.44 +0.22 −0.07 (1σ), E threshold = 1.22 MeV. We have also evaluated the effects of including preliminary Super-Kamiokande data for 1496 days of observations.

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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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Gallium solar neutrino experiments: Absorption cross sections, neutrino spectra, and predicted event rates

Cited by 234 publications

References 55 publications

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

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

Robust signatures of solar neutrino oscillation solutions

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

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