  The main contribution to the pulsar power can be calculated by assuming a
rotating magnetically-dominated magnetosphere described by the force-free
approximation. Although this simple model has been used thoroughly to study
pulsar magnetospheres in the flat spacetime regime, only few works have
considered the relativistic corrections introduced by the curvature and
frame-dragging effects induced by a rotating neutron star. Here we revisit the
problem and describe pulsar magnetospheres within full General Relativity,
quantifying the corrections as a function of the angular velocity, the
compactness of the star and the misalignment angle between the spin and the
magnetic dipole. We provide analytical expressions for the pulsar luminosity by
fitting our numerical results. Finally, we also analyze the effect of the
relativistic corrections on the braking index, which indicates a slight
increment in its value.
