Nuclear symmetry energy and stability of matter in neutron stars

2006/11/23 by S. Kubis, Sebastian Kubis · 3 citations
Physics and Astronomy · #Astrophysics #Atomic and Subatomic Physics Research #Core (optical fiber) #Crust #Gamma-ray bursts and supernovae #Geometry #Geophysics #Neutron #Neutron star #Nuclear drip line #Nuclear matter #Nuclear physics #Nucleon #Nucleosynthesis #Physics #Pulsars and Gravitational Waves Research #Stars #Symmetry (geometry) #astro-ph #r-process

paper · pdf · doi:10.1103/physrevc.76.025801

published as Phys.Rev.C76:025801,2007 · 5 pages, 4 figures

arxiv created 2006/11/23 · openalex publication_date 2007/08/07 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05

Abstract

It is shown that the nuclear symmetry energy is the key quantity in the stability consideration in neutron star matter. The symmetry energy controls the position of crust-core transition and also may lead to new effects in the inner core of neutron star.

Citations

• Determination of the Stiffness of the Nuclear Symmetry Energy from Isospin Diffusion
• Experimental determination of the symmetry energy of a low density nuclear gas
• Isospin asymmetry in nuclei and neutron stars
• Relativistic model for nuclear matter and atomic nuclei with momentum-dependent self-energies

Cited by

• Symmetry energy I: Semi-infinite matter
• Neutron star equilibrium configurations within a fully relativistic theory with strong, weak, electromagnetic, and gravitational interactions
• Exact versus Taylor-expanded energy density in the study of the neutron star crust–core transition