Solar neutrinos: the magnetic moment transition

Details Solar neutrinos: the magnetic moment transition Solar neutrinos: the magnetic moment transition

Jul 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990phlb..244...88p&link_type=abstract

Physics Letters B, Volume 244, Issue 1, p. 88-94.

Physics

2

Scientific paper

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 (105 G)] up to the edge of the convection zone and to decrease linearly, reaching 102 G just below the Sun's surface. The fixed conversion probability lines P(νe --> νμ) (for Majorana neutrinos) and P(νeL --> νμR) (for Dirac neutrinos are obtained on a magnetic moment, mass square difference parameter space (μ, Δ2m21). Two potential solutions are found agreeing with the experimentally acknowledged neutrino flux deficit. They both require μ = (2-4) × 10-10 μB. One is for Δ2m21 ⋍ 3 × 10-4 eV2, corresponding to a resonance near the neutrino production zone in the Sun's core and another for Δ2m21 ⋍ (0.7-1) × 10-8 eV2, corresponding to a resonance in the convection zone. Both cases are adiabatic.

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