Solar Neutrino Flux: Implications of Intrinsic Variability

Details Solar Neutrino Flux: Implications of Intrinsic Variability Solar Neutrino Flux: Implications of Intrinsic Variability

Apr 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aps..apr.x7002c&link_type=abstract

American Physical Society, April Meeting, Jointly Sponsored with the High Energy Astrophysics Division (HEAD) of the American As

Astronomy and Astrophysics

Astrophysics

Scientific paper

The Resonance-Spin-Flavor-Precession (RSFP) process helps explain the evidence for the solar neutrino flux variability presented in the previous abstract. This requires a νe transition magnetic moment as could be found in proposed experiments. The RSFP process gives a good fit to all solar neutrino data. Like the SMA fit, the resonance is near the 0.86 MeV ^7Be line, but the RSFP resonance asymptotes to 1/2, unlike unity for the SMA, so it gives a flat spectrum as measured by the water detectors. The solar rotation rate deduced from the Ga (and also seen in the Cl data) is at a solar density which gives the same E/Δ m^2 value for the resonance position as that required for a fit to all the solar data. This remarkable agreement yields for E=0.86 MeV a Δ m^2 ~ 10-8 eV^2. Details of the flux variability require more complexity than just RSFP, but (as would be expected from the Δ m^2) the MSW LOW solution also contributes. The two overlapping resonances produce the observed bimodal Ga rate distribution, while giving very little variability at the energy of the water detectors where the LOW and RSFP effects are nearly the same.

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