  Some neutron stars may be born spinning fast and with strong magnetic
fields---the so-called \emph{millisecond magnetars}. It is important to
understand how a star's magnetic axis moves with respect to the spin axis in
the star's early life, as this effects both electromagnetic and gravitational
wave emission. Previous studies have highlighted the importance of viscous
dissipation within the star in this process. We advance this program by
additionally considering the effect of the electromagnetic torque. We find an
interesting interplay between the viscous dissipation, which makes the magnetic
axis orthogonalise with respect to the spin, verses magnetic torques that tend
to make the magnetic axis align with the spin axis. We present some results,
and highlight areas where our model needs to be made more realistic.
