On the electrostatic structure of neutron stars

Details On the electrostatic structure of neutron stars On the electrostatic structure of neutron stars

Mar 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aipc.1205..143r&link_type=abstract

THE SUN, THE STARS, THE UNIVERSE AND GENERAL RELATIVITY: International Conference in Honor of Ya.B. Zeldovich's 95th Anniversary

Mathematics

Logic

2

Neutron Stars, Equations Of State, Baryon-Baryon Interactions, Einstein-Maxwell Equations, Neutron Stars, Thermodynamic Functions And Equations Of State, Baryons, Einstein-Maxwell Spacetimes, Spacetimes With Fluids, Radiation Or Classical Fields

Scientific paper

We consider neutron stars composed by, (1) a core of degenerate neutrons, protons, and electrons above nuclear density; (2) an inner crust of nuclei in a gas of neutrons and electrons; and (3) an outer crust of nuclei in a gas of electrons. We use for the strong interaction model for the baryonic matter in the core an equation of state based on the phenomenological Weizsacker mass formula, and to determine the properties of the inner and the outer crust below nuclear saturation density we adopt the well-known equation of state of Baym-Bethe-Pethick. The integration of the Einstein-Maxwell equations is carried out under the constraints of β-equilibrium and global charge neutrality. We obtain baryon densities that sharply go to zero at nuclear density and electron densities matching smoothly the electron component of the crust. We show that a family of equilibrium configurations exists fulfilling overall neutrality and characterized by a non-trivial electrodynamical structure at the interface between the core and the crust. We find that the electric field is overcritical and that the thickness of the transition surface-shell separating core and crust is of the order of the electron Compton wavelength.

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