Talk detail

Participant	Belvedere, Riccardo
Institution	ICRANet Rio - CBPF - Rua Xavier Sigaud, 150 - Urca - Rio de Janeiro - Brazil - Brazil

Session	NS2	Accepted		Order	Time
Talk	Poster abstract	Title	On The Magnetic Field Of Pulsars With Realistic Neutron Star Configurations
Coauthors
Abstract	We have recently developed a neutron star model fulfilling global and not local charge neutrality. The model is described by the coupled Einstein-Maxwell-Thomas-Fermi equations, in which all fundamental interactions are accounted for in the framework of general relativity and relativistic mean field theory. 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 that are very different from estimates based on fiducial parameters for the mass, radius and moment of inertia of the neutron stars. Also, 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. We apply these considerations to the specific high-magnetic field pulsars class and show that, indeed, all of these sources can be described as canonical pulsars driven by the rotational energy of the neutron star, and have magnetic fields lower than the quantum critical field for any value of the neutron star mass.
Pdf file

Session	NS2	Accepted		Order	Time
Talk	Oral abstract	Title	Realistic Neutron Star Configurations and the Magnetic Field of Pulsars
Coauthors
Abstract	We have developed a neutron star (NS) model based on the solution of the coupled Einstein-Maxwell-Thomas-Fermi equations, taking into account all the fundamental interactions in the framework of general relativity and relativistic mean field theory. The model fulfills global and not local charge neutrality and the equilibrium configurations are built both in the static and in the uniformly rotating cases. Uniform rotation is introduced following the Hartle’s formalism. Here, we show that using realistic parameters of rotating neutron stars, are obtained values of the magnetic field and radiation efficiency of pulsars very different from estimates based on fiducial parameters, namely, by assuming a neutron star mass M = 1.4 M⊙, radius R = 10 km, and moment ofinertia I = 10^45 g cm2. In particular, applying realistic values to the high-magnetic field pulsars class, we show that all of these sources can be described as canonical pulsars driven by the rotational energy of the neutron star, and have magnetic fields lower than the quantum critical field for any value of the neutron star mass.
Pdf file