  A statistical analysis of the solar neutrino data is presented assuming the
solar neutrino deficit to be resolved by the resonant interaction of the
neutrino magnetic moment with the solar magnetic field. Four field profiles are
investigated, all exhibiting a rapid increase across the bottom of the
convective zone, one of them closely following the requirements from recent
solar physics investigations. First a 'rates only' analysis is performed whose
best fits appear to be remarkably better than all fits from oscillations. A
global analysis then follows with the corresponding best fits of a comparable
quality to the LMA one. Despite the fact that the resonant spin flavour
precession does not predict any day/night effect, the separate SuperKamiokande
day and night data are included in the analysis in order to allow for a direct
comparison with oscillation scenarios. Remarkably enough, the best fit for
rates and global analysis which is compatible with most astrophysical bounds on
the neutrino magnetic moment is obtained from the profile which most closely
follows solar physics requirements. Allowing for a peak field value of
$3\times10^5G$, it is found in this case that $\Delta
m^2_{21}=1.45\times10^{-8}eV^2$, $\mu_{\nu}=3.2\times10^{-12}\mu_{B}$ (65%CL).
The new forthcoming experiments on solar neutrino physics (Kamland and
Borexino) will be essential to ascertain whether this fact is incidental or
essential.
