On the Magnetic Field of Pulsars with Realistic Neutron Stars Configurations

Understand

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.