2019/01/01 by Jeremy W. Holt, Yeunhwan Lim
Earth and Planetary Sciences · Physics and Astronomy · #Classical mechanics #Equation of state #Gamma-ray bursts and supernovae #High-pressure geophysics and materials #Mean field theory #Moment of inertia #Neutron #Neutron star #Nuclear matter #Nuclear physics #Nuclear structure #Nucleon #Physics #Pulsars and Gravitational Waves Research #Quantum mechanics #Statistical physics #astro-ph.HE #nucl-th
paper · pdf · doi:10.1063/1.5117809
9 pages, 5 figures. To appear in the AIP Proceedings of the Xiamen-CUSTIPEN Workshop on the EOS of Dense Neutron-Rich Matter in the Era of Gravitational Wave Astronomy, Jan. 3-7, Xiamen, China
openalex publication_date 2019/01/01 · arxiv created 2019/04/25 · openalex created_date 2019/07/23 · arxiv updated 2019/09/04 · openalex updated_date 2026/08/05
The equation of state of dense matter determines the structure of neutron stars, their typical radii, and maximum masses. Recent improvements in theoretical modeling of nuclear forces from the low-energy effective field theory of QCD has led to tighter constraints on the equation of state of neutron-rich matter at and somewhat above the densities of atomic nuclei, while the equation of state and composition of matter at high densities remains largely uncertain and open to a multitude of theoretical speculations. In the present work we review the latest advances in microscopic modeling of the nuclear equation of state and demonstrate how to consistently include also empirical nuclear data into a Bayesian posterior probability distribution for the model parameters. Derived bulk neutron star properties such as radii, moments of inertia, and tidal deformabilities are computed, and we discuss as well the limitations of our modeling.