2001/11/12 by F. Douchin, P. Haensel · 14 citations
Earth and Planetary Sciences · Physics and Astronomy · #Gamma-ray bursts and supernovae #High-pressure geophysics and materials #Pulsars and Gravitational Waves Research #astro-ph
paper · pdf · doi:10.1051/0004-6361:20011402
17 pages, 10 figures, latex, uses aa.cls, to be published in Astronomy and Astrophysics
arxiv created 2001/11/12 · openalex publication_date 2001/12/01 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/04
An equation of state (EOS) of neutron star matter, describing both the neutron star crust and the liquid core, is calculated. It is based on the effective nuclear interaction SLy of the Skyrme type, which is particularly suitable for the application to the calculation of the properties of very neutron rich matter (Chabanat et al. 1997, 1998). The structure of the crust, and its EOS, is calculated in the approximation, and under the assumption of the ground state composition. The crust-core transition is a very weakly first-order phase transition, with relative density jump of about one percent. The EOS of the liquid core is calculated assuming (minimal) npeμ composition. Parameters of static neutron stars are calculated and compared with existing observational data on neutron stars. The minimum and maximum masses of static neutron stars are and , respectively. Effects of rotation on the minimum and the maximum mass of neutron stars are briefly discussed.