We derive a new equation of state ( EoS ) for neutron stars ( NS ) from the outer crust to the core based on modern microscopic calculations using the Argonne v _ { 18 } potential plus three-body forces computed with the Urbana model .
To deal with the inhomogeneous structures of matter in the NS crust , we use a recent nuclear energy density functional that is directly based on the same microscopic calculations , and which is able to reproduce the ground-state properties of nuclei along the periodic table .
The EoS of the outer crust requires the masses of neutron-rich nuclei , which are obtained through Hartree-Fock-Bogoliubov calculations with the new functional when they are unknown experimentally .
To compute the inner crust , Thomas-Fermi calculations in Wigner-Seitz cells are performed with the same functional .
Existence of nuclear pasta is predicted in a range of average baryon densities between \simeq 0.067 fm ^ { -3 } and \simeq 0.0825 fm ^ { -3 } , where the transition to the core takes place .
The NS core is computed from the new nuclear EoS assuming non-exotic constituents ( core of npe \mu matter ) .
In each region of the star , we discuss the comparison of the new EoS with previous EoSs for the complete NS structure , widely used in astrophysical calculations .
The new microscopically derived EoS fulfills at the same time a NS maximum mass of 2 M _ { \odot } with a radius of 10 km , and a 1.5 M _ { \odot } NS with a radius of 11.6 km .