  We study the torsional magneto-elastic oscillations of relativistic
superfluid magnetars and explore the effects of a phase transition in the
crust-core interface (nuclear pasta) which results in a weaker elastic
response. Exploring various models with different extension of nuclear pasta
phases, we find that the differences in the oscillation spectrum present in
purely elastic modes (weak magnetic field), are smeared out with increasing
strength of the magnetic field. For magnetar conditions, the main
characteristic and features of models without nuclear pasta are preserved. We
find in general two classes of magneto-elastic oscillations which exhibit a
different oscillation pattern. For B_p < 4 x 10^{14} G, the spectrum is
characterised by the turning points and edges of the continuum which are
confined into the star's core, and have no constant phase. Increasing the
magnetic field, we find, in addition, several magneto-elastic oscillations
which reach the surface and have an angular structure similar to crustal modes.
These global magneto-elastic oscillations show a constant phase and become
dominant when B_p > 5 x 10^{14} G. We do not find any evidence of fundamental
pure crustal modes in the low frequency range (below 200 Hz) for B_p >= 10^{14}
G.
