2013/09/30 by A. Y. Potekhin, A. F. Fantina, N. Chamel +3
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysics #Context (archaeology) #Equation of state #Geophysics #High-pressure geophysics and materials #Inner core #Neutron #Neutron star #Nuclear matter #Nuclear physics #Nuclear physics research studies #Nucleon #Outer core #Parametrization (atmospheric modeling) #Physics #Pulsars and Gravitational Waves Research #Quantum mechanics #Radiative transfer #astro-ph.HE #astro-ph.SR #nucl-th
paper · pdf · doi:10.1051/0004-6361/201321697
published as Astron. Astrophys. 560, A48 (2013) · 13 pages, 10 figures, 10 tables. In v.2, minor typos in the text and references are fixed. In v.3 and v.4, typos in Table 6 and Eq.(17), respectively, are fixed. In v.5, labels on Fig.7 are corrected
openalex publication_date 2013/09/30 · arxiv created 2015/05/13 · arxiv updated 2015/05/14 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Context. An equation of state (EoS) of dense nuclear matter is a prerequisite for studies of the structure and evolution of compact stars. A unified EoS should describe the crust and the core of a neutron star using the same physical model. The Brussels-Montreal group has recently derived a family of such EoSs based on the nuclear energy-density functional theory with generalized Skyrme effective forces that have been fitted with great precision to essentially all the available mass data. At the same time, these forces were constrained to reproduce microscopic calculations of homogeneous neutron matter based on realistic two- and three-nucleon forces.