Solar Physics

, Volume 291, Issue 12, pp 3467–3484 | Cite as

Comparative Analyses of Brookhaven National Laboratory Nuclear Decay Measurements and Super-Kamiokande Solar Neutrino Measurements: Neutrinos and Neutrino-Induced Beta-Decays as Probes of the Deep Solar Interior

  • P. A. SturrockEmail author
  • E. Fischbach
  • J. D. Scargle


An experiment carried out at the Brookhaven National Laboratory over a period of almost 8 years acquired 364 measurements of the beta-decay rates of a sample of \({}^{32}\mbox{Si}\) and, for comparison, of a sample of \({}^{36}\mbox{Cl}\). The experimenters reported finding “small periodic annual deviations of the data points from an exponential decay … of uncertain origin”. We find that power-spectrum and spectrogram analyses of these datasets show evidence not only of the annual oscillations, but also of transient oscillations with frequencies near 11 year−1 and 12.5 year−1. Similar analyses of 358 measurements of the solar neutrino flux acquired by the Super-Kamiokande neutrino observatory over a period of about 5 years yield evidence of an oscillation near 12.5 year−1 and another near 9.5 year−1. An oscillation near 12.5 year−1 is compatible with the influence of rotation of the radiative zone. We suggest that an oscillation near 9.5 year−1 may be indicative of rotation of the solar core, and that an oscillation near 11 year−1 may have its origin in a tachocline between the core and the radiative zone. Modulation of the solar neutrino flux may be attributed to an influence of the Sun’s internal magnetic field by the Resonant Spin Flavor Precession (RSFP) mechanism, suggesting that neutrinos and neutrino-induced beta decays can provide information about the deep solar interior.


Nuclear physics Solar structure 



We acknowledge with thanks the generous cooperation of David Alburger in providing the BNL data and relevant experimental information. We thank the Super-Kamiokande Observatory for making available their solar neutrino measurements. We thank our colleague Guenther Walther for advice concerning the statistical analyses in Section 2 and Section 5. We thank Alexander Parkhomov of the Lomonosov Moscow State University, Heinrich Schrader of the Physikalisch-Technische Bundesanstalt, and Gideon Steinitz of the Geological Survey of Israel, for sharing data with us, which, while not addressed specifically in this article, have provided crucial background information. We thank David Gilbert for assistance in preparing the figures, and we thank an anonymous referee for comments and suggestions that significantly improved the article.

Disclosure of Potential Conflicts of Interest

The authors declare that they have no conflicts of interest.


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Copyright information

© Springer Science+Business Media Dordrecht 2016

Authors and Affiliations

  1. 1.Kavli Institute for Particle Astrophysics and Cosmology and the Center for Space Science and AstrophysicsStanford UniversityStanfordUSA
  2. 2.Department of Physics and AstronomyPurdue UniversityWest LafayetteUSA
  3. 3.NASA/Ames Research Center, MS 245-3Moffett FieldUSA

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