Comparative analysis of GALLEX and GNO solar neutrino data

Sturrock, P. A.; Caldwell, D. O.; Scargle, Jeffrey D.

doi:10.1016/j.astropartphys.2006.06.001

Cited by 22 publications

(38 citation statements)

References 43 publications

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“…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). Since there are important differences between GALLEX and GNO data [for instance, there is a 5-sigma difference in the error estimates (Sturrock, Caldwell, and Scargle 2006)], we analyze these two datasets separately.…”

Section: Gallex and Gno Datamentioning

confidence: 99%

“…Hence evidence for bimodality may be construed as evidence for variability. A possible source of such variability would be rotational modulation, for which we have found evidence in power-spectrum analyses (Sturrock, Caldwell, and Scargle, 2006). It is therefore interesting to compare the power spectra formed from GALLEX runs 1 to 42 and GALLEX runs 42 to 65.…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Gallex and Gno Datamentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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

Sturrock

2008

Sol Phys

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“…To form spectrograms, we first prepare the data by means of the RONO (Rank-Order NOrmalization) operation (Sturrock et al, 2011a) that maps the measurements onto a normal distribution, as is appropriate for power-spectrum analyses such as the Lomb-Scargle procedure (Lomb, 1976;Scargle, 1982) or a likelihood procedure (Sturrock et al, 2006). We then carry out a sequence of likelihood power-spectrum analyses of sections of the data.…”

Section: Analysis Of Ptb Measurementsmentioning

confidence: 99%

Concerning the time dependence of the decay rate of 137Cs

Jenkins

Fischbach

Javorsek

et al. 2013

Applied Radiation and Isotopes

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“…However, the magnetic field at disk center may have roots deep in the convection zone, and possibly removed from the equatorial section. Hence it is worth noting that the synodic rotation rate in an equatorial section of the convection zone covers the range 13.1−13.9 yr −1 , and the synodic rotation rate at latitude 25 o is lower by about 0.3yr −1 (Schou, Christensen-Dalsgaard, and Thompson, 1992 corresponding to the range of synodic rotation rate in a complete equatorial section solar interior (Sturrock, Caldwell, and Scargle, 2006).…”

Section: Power-spectrum Of the Photospheric Magnetic Field For The Ovmentioning

confidence: 99%

Comparative Analysis of Super-Kamiokande and SNO Solar-Neutrino Data and the Photospheric Magnetic Field

Sturrock

2006

Sol Phys

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Abstract. We carry out a comparative analysis of Super-Kamiokande, SNO, and photospheric magnetic-field data for the interval in which these datasets overlap. This proves to be the interval of operation of the D 2 O phase of the SNO experiment. Concerning rotational modulation, we find that the magnetic-field power spectrum shows the strongest peaks at the second and sixth harmonics of the solar synodic rotation frequency [i.e. at 3ν rot and 7ν rot ]. We find that the restricted Super-Kamiokande dataset has a strong modulation at the second harmonic, as we found to be the case for the complete Super-Kamiokande dataset. The SNO D 2 O dataset exhibits weak modulation at that frequency, but shows strong modulation in the band corresponding to the sixth harmonic (too high a frequency to be detectable in the Super-Kamiokande dataset, which is available only in 5-day bins, whereas SNO data is available in one-day bins). We estimate the significance level of the correspondence of the SuperKamiokande second-harmonic peak with the corresponding magnetic-field peak to be 0.0004, and the significance level of the correspondence of the SNO D 2 O sixth-harmonic peak with the corresponding magnetic-field peak to be 0.009. By estimating the amplitude of the modulation of the solar neutrino flux at the second harmonic from the restricted Super-Kamiokande dataset, we find that the weak power at that frequency in the SNO D 2 O power spectrum is not particularly surprising. We also examine power spectra in the neighborhood of 9.43 yr −1 , which is the frequency of a particularly strong modulation in the entire Super-Kamiokande dataset. There is no peak at this frequency in the power spectrum formed from the restricted Super-Kamiokande dataset. It is therefore not surprising that we find (in agreement with the recent analysis by the SNO collaboration) that this peak does not show up in the SNO D 2 O dataset, either.2

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Comparative analysis of GALLEX and GNO solar neutrino data

Cited by 22 publications

References 43 publications

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

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

Concerning the time dependence of the decay rate of 137Cs

Comparative Analysis of Super-Kamiokande and SNO Solar-Neutrino Data and the Photospheric Magnetic Field

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