  We investigate the slowly rotating general relativistic superfluid neutron
stars including the entrainment effect in a two-fluid model, where one fluid
represents the superfluid neutrons and the other is the charge-neutral fluid
called the proton fluid, made of protons and electrons. The equation of state
and the entrainment effect between the superfluid neutrons and the proton fluid
are computed using a relativistic mean field (RMF) model where baryon-baryon
interaction is mediated by the exchange of $\sigma$, $\omega$, and $\rho$
mesons and scalar self interactions are also included. The equations governing
rotating neutron stars in the slow rotation approximation are second order in
rotational velocities of neutron and proton fluids. We explore the effects of
the isospin dependent entrainment and the relative rotation between two fluids
on the global properties of rotating superfluid neutron stars such as mass,
shape, and the mass shedding (Kepler) limit within the RMF model with different
parameter sets. It is observed that for the global properties of rotating
superfluid neutron stars in particular, the Kepler limit is modified compared
with the case that does not include the contribution of $\rho$ mesons in the
entrainment effect.
