  Assuming the solar neutrino deficit is resolved by the resonant interaction
of the neutrino magnetic moment with the solar magnetic field --in the
framework of Resonant Spin Flavour Precession (RSFP) scenario-- the solar
magnetic field profile function has been derived from the scenario in the light
of solar neutrino data. An approximate qualitative analysis has been done for
vanishing vacuum mixing and it has been found that the profile derived is quite
stable in nature. As because on changing the neutrino parameters ($\mu_{\nu},
\Delta{m^2}$) and the solar neutrino data the profile is just scaled along the
axes. In principle, the nature of the profile is strongly dependent on the
solar matter density distribution function. The current approach is quite
different from the usual one- in which the best field profile is discovered by
performing $\chi^{2}_{min.}$ calculations using solar neutrino data.
Furthermore, the profile derived in the present work --when tested by
$\chi^{2}_{min.}$ calculations-- was found to be the best suited one, for the
solar interior.
