  To determine the frequencies of magnetic oscillations in neutron stars with
highly tangled magnetic fields, we derive the perturbation equations. We assume
that the field strength of the global magnetic structure is so small that such
fields are negligible compared with tangled fields, which may still be far from
a realistic configuration. Then, we systematically examine the spectra of the
magnetic oscillations, as varying the magnetic field strength and stellar mass.
The frequencies without crust elasticity are completely proportional to the
strength of the magnetic field, whose proportionality constant depends strongly
on the stellar mass. On the other hand, the oscillation spectra with crust
elasticity become more complicated, where the frequencies even for weak
magnetic fields are different from the crustal torsional oscillations without
magnetic fields. For discussing spectra, the critical field strength can play
an important role, and it is determined in such a way that the shear velocity
is equivalent to the Alfv\'{e}n velocity at the crust basis. Additionally, we
find that the effect of the crust elasticity can be seen strongly in the
fundamental oscillations with a lower harmonic index, $\ell$. Unlike the
stellar models with a pure dipole magnetic field, we also find that the spectra
with highly tangled magnetic fields become discrete, where one can expect many
of the eigenfrequencies. Maybe these frequencies could be detected after the
violent phenomena breaking the global magnetic field structure.
