  We have solved numerically the general relativistic induction equations in
the interior background spacetime of a slowly rotating magnetized neutron star.
The analytic form of these equations was discussed in a recent paper (Rezzolla
et al 2001a), where corrections due both to the spacetime curvature and to the
dragging of reference frames were shown to be present. Through a number of
calculations we have investigated the evolution of the magnetic field with
different rates of stellar rotation, different inclination angles between the
magnetic moment and the rotation axis, as well as different values of the
electrical conductivity. All of these calculations have been performed for a
constant temperature relativistic polytropic star and make use of a consistent
solution of the initial value problem which avoids the use of artificial
analytic functions. Our results show that there exist general relativistic
effects introduced by the rotation of the spacetime which tend to decrease the
decay rate of the magnetic field. The rotation-induced corrections are however
generally hidden by the high electrical conductivity of the neutron star matter
and when realistic values for the electrical conductivity are considered, these
corrections become negligible even for the fastest known pulsar.
