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We have recently developed a neutron star model fulfilling global and notlocal charge neutrality, both in the static and in the uniformly rotatingcases. The model is described by the coupled Einstein-Maxwell-Thomas- Fermi(EMTF) equations, in which all fundamental interactions are accounted for inthe framework of general relativity and relativistic mean field theory. Uniformrotation is introduced following the Hartle's formalism. We show that the useof realistic parameters of rotating neutron stars obtained from numericalintegration of the self-consistent axisymmetric general relativistic equationsof equilibrium leads to values of the magnetic field and radiation efficiencyof pulsars very different from estimates based on fiducial parameters assuminga 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 inferredfrom the traditional Newtonian rotating magnetic dipole model with respect tothe one obtained from its general relativistic analog which takes into dueaccount the effect of the finite size of the source. We apply theseconsiderations to the specific high-magnetic field pulsars class and show that,indeed, all these sources can be described as canonical pulsars driven by therotational energy of the neutron star, and with magnetic fields lower than thequantum critical field for any value of the neutron star mass.

On the Magnetic Field of Pulsars with Realistic Neutron Stars Configurations