Solar Neutrino Data Covering Solar Cycle 22

Fukuda, Y.; Hayakawa, Tomokatsu; Inoue, K.; Ishihara, K.; Ishino, H.; Joukou, S.; Kajita, T.; Kasuga, S.; Koshio, Y.; Kumita, T.; Matsumoto, K.; Nakahata, M.; Nakamura, K.; Okumura, K.; Sakai, Akito; Shiozawa, M.; Suzuki, Junya; Suzuki, Y.; Tomoeda, T.; Totsuka, Y.; Hirata, Keiko; Kihara, K.; Oyama, Y.; Koshiba, M.; Nishijima, K.; Horiuchi, Takashi; Fujita, K.; Hatakeyama, S.; Koga, M.; Maruyama, T.; Mori, M.; Kajimura, T.; Suda, T.; Suzuki, A.; Ishizuka, T.; Miyano, K.; Okazawa, H.; Hara, T.; Nagashima, Y.; Takita, M.; Yamaguchi, Tomohiro; Hayato, Y.; Kaneyuki, K.; Suzuki, T.; Takeuchi, Y.; Tanimori, T.; Tasaka, S.; Ichihara, E.; Miyamoto, S.; Nishikawa, K.

doi:10.1103/physrevlett.77.1683

Cited by 697 publications

(265 citation statements)

References 16 publications

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“…The Kamiokande [28], Super-Kamiokande (SK) [29] and SNO [30] experiments detect neutrino events in real-time by detecting theČerenkov light from electrons recoiling as a consequence of neutrino interactions. In addition, phase III of the SNO experiment uses an array of 3 He proportional counters for neutron detection.…”

Section: Waterčerenkov Experimentsmentioning

confidence: 99%

Measurement of the calorimetric energy scale in MINOS

Hartnell¹

2005

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MINOS is a long-baseline neutrino oscillation experiment. A neutrino beam is created at the Fermi National Accelerator Laboratory in Illinois and fired down through the Earth. Measurements of the energy spectra and composition of the neutrino beam are made both at the source using the Near detector and 735 km away at the Soudan Underground Laboratory in Minnesota using the Far detector. By comparing the spectrum and flavour composition of the neutrino beam between the two detectors neutrino oscillations can be observed. Such a comparison depends on the accuracy of the relative calorimetric energy scale.This thesis details a precise measurement of the calorimetric energy scale of the MINOS Far detector and Calibration detector using stopping muons with a new "track window" technique. These measurements are used to perform the relative calibration between the two detectors. This calibration has been accomplished to 1.7% in data and to significantly better than 2% in the Monte Carlo simulation, thus achieving the MINOS relative calibration target of 2%.A number of cross-checks have been performed to ensure the robustness of the calorimetric energy scale measurements. At the Calibration detector the test-beam energy between run periods is found to be consistent with the detector response to better than 2% after the relative calibration is applied. The muon energy loss in the MINOS detectors determined from Bethe-Bloch predictions, data and Monte Carlo are compared and understood.To estimate the systematic error on the measurement of the neutrino oscillation parameters caused by a relative miscalibration a study is performed. A 2% relative miscalibration is shown to cause a 0.6% bias in the values of ∆m 2 and sin 2 (2θ).To my parents.i

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Section: Waterčerenkov Experimentsmentioning

confidence: 99%

Measurement of the calorimetric energy scale in MINOS

Hartnell¹

2005

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“…The KamLAND detector [11,52], located in the site of the famous Kamiokande experiment [53], consists of approximately one kton of liquid scintillator surrounded by photomultiplier tubes. KamLAND is sensitive to theν e flux, ν e + p → n + e + , (6.1) from 17 reactors that are located reasonably close to the detector.…”

Section: Predictions For Kamland Reactor Experimentsmentioning

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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“…The benefit of adding 35 Cl is two-fold. Since 35 Cl has a (n,γ) cross section which is over 80,000 times larger than that of 2 H, more neutrons will capture within the D 2 O region [60].…”

Section: Neutrino Interactions In Snomentioning

confidence: 99%

“…Since 35 Cl has a (n,γ) cross section which is over 80,000 times larger than that of 2 H, more neutrons will capture within the D 2 O region [60]. Also, a neutron capture on 35 Cl results in a cascade of γ-rays with a total energy of 8.6 MeV, allowing more of the neutron interactions to be observed above the detector energy threshold.…”

Section: Neutrino Interactions In Snomentioning

confidence: 99%