RSFP PREDICTIONS FOR TRANSVERSE SOLAR MAGNETIC-FIELD DISTRIBUTION FROM SOLAR-NEUTRINO DATA

Even though the standard solar model (SSM) has been very successful in predicting the thermal and nuclear evolution of the Sun, it does not throw enough light on solar magnetic activity. In the absence of a gen erally accepted theory of solar dynamo, various general arguments have been put forth to constrain solar magnetic fields. In the absence of reliable knowledge of solar magnetic fields from available astrophysic al data, it may be worthwhile to constrain the solar magnetic fields f rom solar neutrino observations assuming Resonant Spin-Flavor Precessi on (RSFP) to be responsible for the solar neutrino deficit. The config uration of solar magnetic field derived in this work is in reasonably good agreement with the magnetic field distribution proposed by Akhmed ov et al. (Sov. Phys. JETP 68, 250 (1989)). However, the magnetic fiel d distribution in the radiation zone used by Pulido (Phys. Rep. 211, 1 67 (1992)) is ruled out. The magnitude of the magnetic field in the ra diation and convective zones of the Sun are very sensitive to the valu e chosen for the neutrino magnetic moment. However, any change in the value of neutrino magnetic moment does not affect the magnetic field d istribution as it only scales the magnetic field strength at different points by the same amount.