From the crust to the core of Neutron Stars on a microscopic basis
arXiv:1308.2304 · doi:10.1134/S1063778814080031
Abstract
Within a microscopic approach the structure of Neutron Stars is usually studied by modelling the homogeneous nuclear matter of the core by a suitable Equation of State, based on a many-body theory, and the crust by a functional based on a more phenomenological approach. We present the first calculation of Neutron Star overall structure by adopting for the core an Equation of State derived from the Brueckner-Hartree-Fock theory and for the crust, including the pasta phase, an Energy Density Functional based on the same Equation of State, and which is able to describe accurately the binding energy of nuclei throughout the mass table. Comparison with other approaches is discussed. The relevance of the crust Equation of state for the Neutron Star radius is particularly emphasised.
14 pages, 6 figures, accepted version
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- Are nuclear matter properties correlated to neutron star observables ?
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- Structure and composition of inner crust of neutron stars from Gogny interactions
- Exact versus Taylor-expanded energy density in the study of the neutron star crust-core transition
- Extended Skyrme Equation of State in asymmetric nuclear matter
- Microscopic nuclear equation of state at finite temperature and stellar stability
- Cooling of hybrid neutron stars with microscopic equations of state
- Tetraneutron condensation in neutron rich matter
- Non-radial oscillations and gravitational wave emission of hybrid neutron stars
- Nuclear Pairing Gaps and Neutron Star Cooling
- Neutron star cooling and mass distributions
- Cooling of dark neutron stars
- Properties of rapidly rotating hot neutron stars within Brueckner theory