Abstract
The resonant spin flip flavour precession of solar neutrinos, a combined effect of matter and magnetic field, is reexamined. The solar magnetic field in the Sun's interior is assumed to be constant [O (10 5 G)] up to the edge of the convection zone and to decrease linearly, reaching 10 2 G just below the Sun's surface. The fixed conversion probability lines P(ν e → ν μ) (for Majorana neutrinos) and P( ν eL → ν μR ) (for Dirac neutrinos are obtained on a magnetic moment, mass square difference parameter space ( μ, Δ 2 m 21). Two potential solutions are found agreeing with the experimentally acknowledged neutrino flux deficit. They both require μ = (2−4) × 10 −10 μ B. One is for Δ 2m 21 ⋍ 3 × 10 −4 eV 2 , corresponding to a resonance near the neutrino production zone in the Sun's core and another for Δ 2m 21 ⋍ (0.7−1) × 10 −8 eV 2 , corresponding to a resonance in the convection zone. Both cases are adiabatic.
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