  We have recently developed a neutron star model fulfilling global and not
local charge neutrality, both in the static and in the uniformly rotating
cases. The model is described by the coupled Einstein-Maxwell-Thomas- Fermi
(EMTF) equations, in which all fundamental interactions are accounted for in
the framework of general relativity and relativistic mean field theory. Uniform
rotation is introduced following the Hartle's formalism. We show that the use
of realistic parameters of rotating neutron stars obtained from numerical
integration of the self-consistent axisymmetric general relativistic equations
of equilibrium leads to values of the magnetic field and radiation efficiency
of pulsars very different from estimates based on fiducial parameters assuming
a neutron star mass, M = 1.4 Msun, radius R = 10 km, and moment of inertia, I =
10^45 g cm^2. In addition, we compare and contrast the magnetic field inferred
from the traditional Newtonian rotating magnetic dipole model with respect to
the one obtained from its general relativistic analog which takes into due
account the effect of the finite size of the source. We apply these
considerations to the specific high-magnetic field pulsars class and show that,
indeed, all these sources can be described as canonical pulsars driven by the
rotational energy of the neutron star, and with magnetic fields lower than the
quantum critical field for any value of the neutron star mass.
