Implications of the GALLEX determination of the solar neutrino flux
The GALLEX result 83 ± 19 (stat.) ± 8 (syst.) SNU is two standard deviations below the predictions of stellar model calculations (124-132 SNU). To fit this result together with those of the chlorine and Kamiokande experiments requires severe stretching of solar models but does not rule out such a pr...
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| Main Authors: | , , , , , , , , , , , |
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| Format: | Article (Journal) |
| Language: | English |
| Published: |
1992
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| In: |
Physics letters
Year: 1992, Volume: 285, Issue: 4, Pages: 390-397 |
| ISSN: | 1873-2445 |
| DOI: | 10.1016/0370-2693(92)91522-B |
| Online Access: | Verlag, lizenzpflichtig, Volltext: https://doi.org/10.1016/0370-2693(92)91522-B Verlag, lizenzpflichtig, Volltext: https://www.sciencedirect.com/science/article/pii/037026939291522B 
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| Author Notes: | P. Anselmann, W. Hampel, G. Heusser, J. Kiko, T. Kirsten, E. Pernicka, R. Plaga, U. Rönn, M. Sann, C. Schlosser, R. Wink, M. Wójcik, R. von Ammon, K. H. Ebert, E. Henrich, M. Balata, E. Bellotti, N. Ferrari, H. Lalla, T. Stolarczyk, C. Cattadori, O. Cremonesi, E. Fiorini, S. Pezzoni, L. Zanotti, F. von Feilitzsch, R. Mößbauer, U. Schanda, G. Berthomieu, E. Schatzman, I. Carmi, I. Dostrovsky, C. Bacci, P. Belli, R. Bernabei, S. d'Angelo, L. Paoluzi, S. Charbit, M. Cribier, G. Dupont, L. Gosset, J. Rich, M. Spiro, C. Tao, D. Vignaud, R.L. Hahn, F.X. Hartmann, J.K. Rowley, R.W. Stoenner, J. Weneser |
MARC
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| 520 | |a The GALLEX result 83 ± 19 (stat.) ± 8 (syst.) SNU is two standard deviations below the predictions of stellar model calculations (124-132 SNU). To fit this result together with those of the chlorine and Kamiokande experiments requires severe stretching of solar models but does not rule out such a procedure, leaving the possibility of massless neutrinos. It clearly implies that the pp neutrinos have been detected. The Mikheyev-Smirnov-Wolfenstein (MSW) mechanism provides a good fit, and the GALLEX result fixes the Δm2 and sin2 2θ parameters in two very confined ranges (around Δm2 = 6 × 10−6eV2 and sin2 2θ = 7 × 10−3 and around Δm2 = 8 × 10−6eV2 and sin2 2θ = 0.6). Explanations of the solar neutrino problems based on the decay or magnetic interactions of neutrinos are disfavoured. | ||
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