  We study the dynamics of r-modes in the ocean of a magnetic neutron star. We
modeled the star's ocean with a spherical rotating thin shell and assumed that
the magnetic field symmetry axis is not aligned to the shell's spin axis. In
the magnetohydrodynamic approximation, we calculate the frequency of $\ell=m$
r-modes in the shell of an incompressible fluid. Different r-modes with $\ell$
and $\ell\pm2$ are coupled by the {\it inclined} magnetic field. Kinematical
secular effects for the motion of a fluid element in the shell undergoing
$\ell=m=2$ r-mode are studied. The magnetic corrected drift velocity of a given
fluid element undergoing the $\ell=m$ r-mode oscillations is obtained. The
magnetic field increases the magnitude of the fluid drift produced by the
r-mode drift velocity, the high-$\ell$ modes in the ocean fluid will damp
faster than the low-$\ell$ ones.
