  It is shown that in the presence of a background magnetic field within solar
interior a cavity for low frequency MHD eigen modes (with periods 1-10 days)
near equatorial plane can arise. The lower boundary of the cavity coincides
with the centre of the Sun while the upper one corresponds to the Alfven
resonant layer where high accumulation of wave energy takes place. The
localization and the width of the Alfven resonance layer are determined by: (i)
the node number of eigen modes n = 1, 2,..., (ii) by the angle of oblique
propagation of waves with respect to the magnetic field, and (iii) by a low
magnitude of the background magnetic field itself, B=1-100 G. The amplitude of
eigen oscillations in a resonant layer determines the density fluctuation value
that is restricted through the imaginary part of eigen frequences. For large
node numbers n>>1 there appear many narrow resonant layers where a neutrino
propagates through a large density fluctuation \delta\rho/\rho with the
oscillation length that is much bigger than the width of a resonant layer. It
is shown that neutrino crosses many such bumps on the exponential background
profile that motivates to consider these MHD waves as a plausible matter noise
for the MSW solution to the Solar Neutrino Problem (SNP).
