GALLEX solar neutrino observations. The results from GALLEX I and early results from GALLEX II

Anselmann, P.; Hampel, W.; Heusser, G.; Kiko, J.; Kirsten, T.; Laubenstein, M.; Pernicka, Ernst; Pezzoni, S.; Plaga, R.; Rönn, U.; Sann, M.; Schlosser, C.; Wink, R.; Wójcik, M.; Ammon, R. von; Ebert, Klaus; Fritsch, Tobias; Hellriegel, K.; Henrich, Ε.; Stieglitz, L.; Weyrich, F.; Balata, M.; Ferrari, Nicola; Lalla, H.; Bellotti, E.; Cattadori, C.; Cremonesi, O.; Fiorini, E.; Zanotti, L.; Altmann, M.; Feilitzsch, F. von; Möβbauer, R.; Schanda, Ulrich; Berthomieu, G.; Schatzman, E.; Carmi, Israel; Dostrovsky, I.; Bacci, C.; Belli, P.; Bernabei, R.; d’Angelo, S.; Paoluzi, L.; Charbit, S.; Cribier, M.; Dupont, Graham; 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(93)91264-n

Cited by 130 publications

(48 citation statements)

References 15 publications

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“…Fluctuations on the time scale of a radiochemical experiment's run would broaden the distribution of count rates, since different runs would have different survival probabilities. None of the experiments currently operating has noted a broader distribution of rates than expected [13,14,15], suggesting that the neutrino data will probably limit, rather than measure, such fluctuations. For the favored, small-angle solution, the variance is strongly peaked when neutrinos are produced near the resonance.…”

Section: Discussionmentioning

confidence: 98%

MSW effect in a fluctuating matter density

1996

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We consider the effect on matter-enhanced neutrino flavor transformation of a randomly fluctuating, ␦-correlated matter density. The fluctuations will produce a distribution of neutrino survival probabilities. We find the mean and variance of the distribution for the case of solar neutrinos, and discuss the possibility of placing a limit on solar density fluctuations using neutrino data. ͓S0556-2821͑96͒03518-7͔

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Section: Discussionmentioning

confidence: 98%

MSW effect in a fluctuating matter density

1996

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“…We now have available 65 measurements in the GALLEX series (GALLEX I: Anselmann et al, 1993;GALLEX II: Anselmann et al, 1995;Kirsten et al, 1995; GALLEX III: Hampel et al, 1996;GALLEX IV: Hampel et al, 1999) and 58 in the GNO series (Altmann et al, 2000;Kirsten et al, 2003;Altmann et al, 2005). We have taken data from the tables in these articles, except that, for run 42, we adopt for the lower error estimate the value 50 shown in Figure 1 of Hampel et al (1999), rather than the earlier zero value in Table 3 of Hampel et al (1996).…”

Section: Gallex and Gno Datamentioning

confidence: 99%

Analysis of Bimodality in Histograms Formed from GALLEX and GNO Solar Neutrino Data

Sturrock

2008

Sol Phys

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Abstract.A histogram display of the solar neutrino capture-rate measurements made by the GALLEX experiment appears to be bimodal, but that of the follow-on GNO experiment does not. To assess the significance of these results, we introduce a "bimodality index" based on the probability-transform procedure. This confirms that the GALLEX measurements are indeed bimodal (at the 99.98 percent confidence level), and that the GNO measurements are not. Tracking the bimodality index as a function of time shows that the strongest contribution to bimodality comes from runs 42 to 62, i.e. from the time interval 1995.1 to 1996.9. The bimodality index for the first half (runs 1 through 33) is 2.56, whereas that for the second half (runs 33 through 65) is 7.05. Power-spectrum analysis shows a similar distinction: the peaks in the power spectrum formed from the second half are stronger than those in the power spectrum formed from the first half, suggesting that bimodality and rotational modulation are related.2

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“…For example, despite the ∼ tenfold difference between their thresholds of 7.3 and 0.8 MeV, respectively, Kamiokande and Homestake find similar capture rates (Davis 1994). While both of these are still well below that predicted, experiments sensitive to lower energy thresholds, SAGE (Abdurashitov et al 1994) and GALLEX (Anselmann et al 1993), detect rates closer to theoretical predictions. Barring experimental error this would indicate a maximum in the 'missing neutrino spectrum' near the 1-7 MeV range.…”

Section: Introductionmentioning

confidence: 57%

Interactions between solar neutrinos and solar magnetic fields

Oakley

Snodgrass

1997

Astroparticle Physics

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We attempt to correlate all of the available solar-neutrino capture-rate data with the strong magnetic fields these neutrinos encounter in the solar interior along their Earth-bound path. We approximate these fields using the (photospheric, magnetograph-measured) surface magnetic flux from central latitude bands, time delayed to proxy the solar interior. Our strongest evidence for anticorrelation is for magnetic fields within the central ±5 0 solar-latitude band that have been delayed by 0.34 years. Assuming a neutrino-magnetic interaction, this might indicate that interior fields travel to the solar surface in this period of time. As more solar-neutrino flux information is gathered, the question of whether such evidence is physical or statistical in nature should be resolved, providing that new data span enough solar cycles and that correlation studies focus on these isolated fields.

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GALLEX solar neutrino observations. The results from GALLEX I and early results from GALLEX II

Cited by 130 publications

References 15 publications

MSW effect in a fluctuating matter density

MSW effect in a fluctuating matter density

Analysis of Bimodality in Histograms Formed from GALLEX and GNO Solar Neutrino Data

Interactions between solar neutrinos and solar magnetic fields

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