On the fourier spectrum analysis of the solar neutrino capture rate

Abstract

Periodic variations in Davis' experimental data concerning the solar neutrino capture rate are derived on the basis of a Fourier spectrum analysis. Variations in the 37Ar production rate are obtained for a series of randomly spaced observations in the period 1970-1985 (runs 18-89). The harmonic analysis of runs 18-89 has determined solar neutrino capture rate variations with periods of 8.33, 5.00, 2.13, 1.61, 0.83, 0.61, 0.54, and 0.51 yr, thereby confirming earlier calculations performed for the set of runs 18-69 (1983), 18-74 (1985a), and 18-80 (1985b). The results also confirm those of Sakurai (1979) who showed that there is strong evidence that the observed solar neutrino flux has a tendency to vary with quasi-biennial periodicity. We show that the results of the Fourier spectrum analysis do not depend upon certain high or low values in Davis' experimental data.

Solar Neutrino Variability and Its Implications for Solar Physics and Neutrino Physics

“…Our approach has been primarily to apply power spectrum analysis -see, for instance, Sturrock et al (1997), applied to Homestake data; Sturrock, Caldwell & Scargle (2006) and Sturrock (2008a), applied to GALLEX-GNO data; , applied to Super-Kamiokande data; and Sturrock (2006), applied to SNO data. Similar analyses have been carried out by several other authors (Haubold & Gerth 1990;Gavryusev et al 1991;Vasiliev & Ogurtsov 1995;Rivin & Obridko 1997;Kolomeets et al 1998;Shirai 2004;Nakahata et al 2005;and Ranucci 2006). These results also have not been generally accepted as providing convincing evidence of variability.…”

Fourier spectrum analysis of the new solar neutrino capture rate data for the Homestake experiment

“…The graph indicates whether or not there is a periodicity at a given time of the given frequency. π < 1 1 ≤ π < 2 2 ≤ π < 3 3 ≤ π < 4 No.runs Fourier 18-69 0.7 1.63 2.14 3.00 (1970)(1971)(1972)(1973)(1974)(1975)(1976)(1977)(1978)(1979)(1980)(1981) 0.5 1.30 Fourier 0.83 1.61 2.13 18-89 0.61 (1970)(1971)(1972)(1973)(1974)(1975)(1976)(1977)(1978)(1979)(1980)(1981)(1982)(1983)(1984)(1985) 0.54 0.51 Lomb-Scargle 0.7 1.30 18-109 0.54 Fourier 0.7 1.75 2.04 18-133 0.55 1.59 0.53 0.51 Wavelet 0.85 1.89 18-133 0.51 π[yr] 4 ≤ π < 5 5 ≤ π < 6 8 ≤ π < 9 9 ≤ π < 10 No.runs Fourier 8.33 18-69 4.90 (197018-69 4.90 ( -198118-69 4.90 ( ) Fourier 8.33 18-89 (197018-69 4.90 ( -1985 Lomb -Scargle 4.80 9.60 18-109 (1970-1990) Fourier 4.55 18-133 (1970-1994 Wavelet 4.76 18-133 (1970-1994)…”

Analysis of Solar Neutrino Data from Super-Kamiokande I and II

“…If such a variability over time would be discovered, for example, in the Borexino experiment, a mechanism for a chronometer for solar variability could be proposed based on relations between the properties of thermonuclear fusion and g-modes. All the above findings encouraged the conclusion that Fourier and wavelet analysis, which are based upon the analysis of the variance of the respective time series (standard deviation analysis (SDA)) [37,38], should be complemented by the utilization of diffusion entropy analysis (DEA), which measures the scaling of the probability density function (pdf) of the diffusion process generated by the time series, thought of as the physical source of fluctuations [39,40]. For this analysis, we have used the publicly available data of Super-Kamiokande I and Super-Kamiokande II (see Figure 2).…”