Random magnetic fields in the sun and solar neutrinos

Details Random magnetic fields in the sun and solar neutrinos Random magnetic fields in the sun and solar neutrinos

Jun 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991phlb..262..303n&link_type=abstract

Physics Letters B, Volume 262, Issue 2-3, p. 303-306.

Physics

13

Scientific paper

We reconsider the neutrino spin precession in the magnetic field of the sun taking into account the spatial intermittency of the solar magnetic field. The toroidal magnetic field encountered by the neutrino in the solar convection zone is written as the sum of a constant field (B0) on a large scale and a randomly fluctuating field (B1) on a small scale. The resulting stochastic differential equation for spin precession is solved and we find out that for strong random magnetic fields the survival probability P(νe--> νe) is equal to one half. Neutrinos arriving on earth around June 6 or December 8 are traversing the solar equator, where B0 = 0, and by studying this neutrino signal we can isolate the effect of the random component of the solar magnetic field.
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