GALLEX results from the first 30 solar neutrino runs

Anselmann, P.; Hampel, W.; Heusser, G.; Kiko, J.; Kirsten, T.; Laubenstein, M.; Pernicka, Ernst; Pezzoni, S.; Rönn, U.; Sann, M.; Schlosser, C.; Wink, R.; Wójcik, M.; Ammon, R. von; Ebert, Klaus; Fritsch, Tobias; Hellriegel, K.; Henrich, Ε.; Stieglitz, L.; Weirich, F.; Balata, M.; Ferrari, Nicola; Lalla, H.; Bellotti, E.; Cattadori, C.; Cremonesi, O.; Fiorini, E.; Zanotti, L.; Altmann, M.; Feilitzsch, F. von; Mößbauer, R. L.; Schanda, Ulrich; Berthomieu, G.; Schatzman, E.; Carmi, Israel; Dostrovsky, I.; Bacci, C.; Belli, P.; Bernabei, R.; d’Angelo, S.; Paoluzi, L.; Bévilacqua, A.; Charbit, S.; Cribier, M.; Gösset, L.; Rich, J.; Spiro, M.; Stolarczyk, Th.; Tao, C.; Vignaud, D.; Hahn, R. L.; Hartmann, F.; Rowley, J.K.; Stoenner, R.W.; Weneser, J.

doi:10.1016/0370-2693(94)90744-7

Cited by 228 publications

(65 citation statements)

References 23 publications

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“…The counter and electronics improvements made at the start of stage II should permit L-peak events to be included, but no results have been announced as of December, 1994. The corresponding results for GALLEX I (first 15 runs) and II (8/92-10/93) is (Anselmann et al 1994) σφ 71 Ge = 79 ± 10 ± 6 SNU (1σ). (Anselmann et al 1995), R = 1.04 ± 0.12 (1σ).…”

Section: The Sage and Gallex Experimentsmentioning

confidence: 84%

The Solar Neutrino Problem

Haxton¹

1995

Annu. Rev. Astron. Astrophys.

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The solar neutrino problem has persisted for almost three decades. Recent results from Kamiokande, SAGE, and GALLEX indicate a pattern of neutrino fluxes that is very difficult to reconcile with plausible variations in standard solar models. This situation is reviewed and suggested particle physics solutions are discussed. A summary is given of the important physics expected from SNO, SuperKamiokande, and other future experiments.

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Section: The Sage and Gallex Experimentsmentioning

confidence: 84%

The Solar Neutrino Problem

Haxton¹

1995

Annu. Rev. Astron. Astrophys.

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“…The deficit of neutrinos coming from the sun, known as the solar neutrino problem, has long been established by past experiments [1][2][3][4]. A global analysis of these experimental results suggests an energy dependent suppression in the flux of solar neutrinos [5].…”

Section: Introductionmentioning

confidence: 99%

16N as a calibration source for Super-Kamiokande

Blaufuss¹,

Guillian²,

Fukuda³

et al. 2001

Nuclear Instruments and Methods in Physics Research Section A:

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2The decay of 16 N is used to cross check the absolute energy scale calibration for solar neutrinos established by the electron linear accelerator (LINAC). A deuterium-tritium neutron generator was employed to create 16 N via the (n,p) reaction on 16 O in the water of the detector. This technique is isotropic and has different systematic uncertainties than the LINAC. The results from this high statistics data sample agree with the absolute energy scale of the LINAC to better than 1%. A natural source of 16 N from the capture of µ − on 16 O, which is collected as a background to the solar neutrino analysis, is also discussed.

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“…Solar neutrinos have been detected using chlorine-, gallium-, and water-based detectors [1,2,3,4,5]; all have measured significantly lower solar neutrino flux than predicted by Standard Solar Models (SSMs) [6,7,8]. This disagreement between the measured and expected solar neutrino flux, known as the "solar neutrino problem", is generally believed to be due to neutrino flavor oscillations.…”

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confidence: 99%

SolarB8and hep Neutrino Measurements from 1258 Days of Super-Kamiokande Data

Fukuda¹,

Fukuda²,

Ishitsuka³

et al. 2001

Phys. Rev. Lett.

1,064

695

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Solar neutrino measurements from 1258 days of data from the Super-Kamiokande detector are presented [? ]. The measurements are based on recoil electrons in the energy range 5.0-20.0 MeV. The measured solar neutrino flux is 2.32 ± 0.03 (stat.) +0.08 −0.07 (sys.) ×10 6 cm −2 s −1 , which is 45.1 ± 0.5 (stat.) +1.6 −1.4 (sys.)% of that predicted by the BP2000 SSM. The day vs night flux asymmetry (Φn − Φ d )/Φaverage is 0.033 ± 0.022 (stat.) +0.013 −0.012 (sys.). The recoil electron energy spectrum is consistent with no spectral distortion (χ 2 /d.o.f. = 19.0/18). The seasonal variation of the flux is consistent with that expected from the eccentricity of the Earth's orbit (χ 2 /d.o.f. = 3.7/7). For the hep neutrino flux, we set a 90% C.L. upper limit of 40 × 10 3 cm −2 s −1 , which is 4.3 times the BP2000 SSM prediction.22 This preprint is almost identical to the report submitted to Physical Review Letter. We have added to this preprint a few tables of

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GALLEX results from the first 30 solar neutrino runs

Cited by 228 publications

References 23 publications

The Solar Neutrino Problem

The Solar Neutrino Problem

16N as a calibration source for Super-Kamiokande

SolarB8and hep Neutrino Measurements from 1258 Days of Super-Kamiokande Data

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