their analytical solutions also reveal the existence of a spectrum of modes which are absent in a single fluid star. Nonradial oscillations of non-rotating superfluid neutron stars were computed by Lee, whose numerical solutions for the radial and non-radial pulsations of the two-fluid stars identified distinct superfluid modes [@UMIN]. The effects of shear viscosity of the electron fluid and mutual friction on the r-mode oscillations were studied by Lindblom and Mendell [@LINDBLOM2] by constructing an energy functional and computing the time-scales associated with the dissipative terms. The oscillation modes of superfluid analogs of the classical Maclaurin, Jacobi and Roche ellipsoids were derived recently by Sedrakian and Wasserman [@SW2000] within the tensor virial method. The oscillation modes of superfluid ellipsoids separate into two classes corresponding to relative and co-moving (or center-of-mass, hereafter referred as CM) motions of two fluids. The CM oscillations are identical to the oscillations of single-fluid ellipsoids and are undamped if one ignores the viscosity of the normal fluid. The mutual friction contributes only to the damping of the relative oscillation modes. One important feature of the latter modes is that they do not emit gravitational radiation as there is no mass transport associated with them. Our discussion 