Resonant Spin-Flavor Precession Solution to the Solar Neutrino Problem and electron antineutrinos from the Sun

Details Resonant Spin-Flavor Precession Solution to the Solar Neutrino Problem and electron antineutrinos from the Sun Resonant Spin-Flavor Precession Solution to the Solar Neutrino Problem and electron antineutrinos from the Sun

2000-02-16

arxiv.org/abs/hep-ph/0002174v1

Physics

High Energy Physics

High Energy Physics - Phenomenology

6 pages, LaTeX, 2 postsript figures. Talk given at the Xth Baksan School "Particles and Cosmology", 19-25 April 1999, Baksan V

Scientific paper

We have found allowed squared mass difference, magnetic field, mixing angle - regions for the Resonant Spin-Flavor Precession Solution to the Solar Neutrino Problem fitted with the data of all acting solar neutrino experiments. The typical mass difference region varying in dependence on the mixing angle is allowed for some discrete magnetic field regions in a wide range for the fixed neutrino transition magnetic moment. Except of the first allowed range with the lowest field strength the magnetic field amplitude within other discrete allowed regions depend essentially on the shape of a regular magnetic field profile in the convective zone of the Sun. For the non-zero neutrino mixing one can find at 99.9% C.L. an upper limit on the mixing, originated by the non-observation of electron antineutrinos in the SuperKamiokande detector. This limit occurs also sensitive to the magnetic field profile. While at 67% C.L. there is another more stringent upper limit coming from inconsistency of the gallium experiments with others. A new allowed region appears in the case of an additional assumption that the Homestake data are 1.3 times less than the experimental event rate.

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