2020/11/30 by Soonchul Choi, Soon-Chul Choi, Tsuyoshi Miyatsu +2 · 27 citations
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysics #Equation of state #Gamma-ray bursts and supernovae #High-pressure geophysics and materials #Isospin #Neutron #Neutron star #Nuclear astrophysics #Nuclear drip line #Nuclear matter #Nuclear physics #Nucleon #Physics #Pulsars and Gravitational Waves Research #Quantum mechanics #Stars #Symmetry (geometry) #astro-ph.HE #nucl-th
paper · pdf · doi:10.3847/1538-4357/abe3fe
published in The Astrophysical Journal 909(2), 156 (IOP Publishing) · 15 pages, 13 figures
arxiv created 2020/11/30 · openalex publication_date 2021/03/01 · arxiv updated 2021/03/18 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06
Abstract Taking into account the terrestrial experiments and the recent astrophysical observations of neutron stars and gravitational-wave signals, we impose restrictions on the equation of state (EoS) for isospin-asymmetric nuclear matter. Using the relativistic mean-field model with SU(3) flavor symmetry, we investigate the impacts of effective nucleon mass, nuclear incompressibility, and slope parameter of nuclear symmetry energy on the nuclear and neutron star properties. It is found that the astrophysical information of massive neutron stars and tidal deformabilities, as well as the nuclear experimental data, plays an important role to restrict the EoS for neutron stars. In particular, the softness of the nuclear EoS due to the existence of hyperons in the core gives stringent constraints on those physical quantities. Furthermore, it is possible to put limits on the curvature parameter of nuclear symmetry energy by means of nuclear and astrophysical calculations.