  We numerically calculate equilibrium configurations of uniformly rotating and
charged neutron stars, in the case of insulating material and neglecting the
electromagnetic forces acting on the equilibrium of the fluid. This allows us
to study the behaviour of the gyromagnetic ratio for those objects, when
varying rotation rate and equation of state for the matter. Under the
assumption of low charge and incompressible fluid, we find that the
gyromagnetic ratio is directly proportional to the compaction parameter M/R of
the star, and very little dependent on its angular velocity. Nevertheless, it
seems impossible to have g=2 for these models with low charge-to-mass ratio,
where matter consists of a perfect fluid and where the collapse limit is never
reached.
