  The I-Love-Q relations are approximate equation-of-state independent
relations that connect the moment of inertia, the spin-induced quadrupole
moment, and the tidal deformability of neutron stars. In this paper, we study
the I-Love-Q relations for superfluid neutron stars for a general relativistic
two-fluid model: one fluid being the neutron superfluid and the other a
conglomerate of all charged components. We study to what extent the two-fluid
dynamics might affect the robustness of the I-Love-Q relations by using a
simple two-component polytropic model and a relativistic mean field model with
entrainment for the equation-of-state. Our results depend crucially on the spin
ratio $\Omega_{\rm n}/\Omega_{\rm p}$ between the angular velocities of the
neutron superfluid and the normal component. We find that the I-Love-Q
relations can still be satisfied to high accuracy for superfluid neutron stars
as long as the two fluids are nearly co-rotating $\Omega_{\rm n}/\Omega_{\rm p}
\approx 1$. However, the deviations from the I-Love-Q relations increase as the
spin ratio deviates from unity. In particular, the deviation of the Q-Love
relation can be as large as $O(10\%)$ if $\Omega_{\rm n}/\Omega_{\rm p}$ differ
from unity by a few tens of percent. As $\Omega_{\rm n}/\Omega_{\rm p} \approx
1$ is expected for realistic neutron stars, our results suggest that the
two-fluid dynamics should not affect the accuracy of any gravitational waveform
models for neutron star binaries that employ the relation to connect the
spin-induced quadrupole moment and the tidal deformability.
