2004/05/31 by N. Chamel, Nicolas Chamel · 4 citations
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysics #High-pressure geophysics and materials #Neutron #Neutron scattering #Neutron star #Nuclear physics #Nuclear reaction #Physics #Pulsars and Gravitational Waves Research #Quantum, superfluid, helium dynamics #astro-ph #nucl-th #r-process #s-process
paper · pdf · doi:10.1016/j.nuclphysa.2004.09.011
published as Nucl.Phys. A747 (2005) 109-128 · 25 pages, 20 figures, revised published version
openalex publication_date 2004/10/12 · arxiv created 2004/12/01 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
The outer layers of a neutron star are supposed to be formed of a solid Coulomb lattice of neutron rich nuclei. At densities above neutron drip density (about one thousandth of nuclear saturation density), this lattice is immersed in a neutron fluid. Bragg scattering of those dripped neutrons by the nuclei which has been usually neglected is investigated, within a simple mean field model with Bloch type boundary conditions. The main purpose of this work is to provide some estimates for the entrainment coefficients, as required for hydrodynamical two fluid simulations of neutron star crust, which relate the momentum of one fluid to the particle currents of the other two fluids. The implications for the equilibrium neutron star crust structure are also briefly discussed.