2007/10/02 by Plamen Krastev, Plamen G. Krastev, Francesca Sammarruca +6
Physics and Astronomy · #Astrophysics #Atomic and Subatomic Physics Research #Equation of state #FOS: Physical sciences #Gamma-ray bursts and supernovae #Isospin #Neutron #Neutron star #Nuclear Theory (nucl-th) #Nuclear astrophysics #Nuclear matter #Nuclear physics #Nucleon #Physics #Pulsars and Gravitational Waves Research #Quantum mechanics #nucl-th
paper · pdf · doi:10.48550/arxiv.0710.0427
Contribution to the Twenty Sixth International Workshop on Nuclear Theory held in Rila Mountains, Bulgaria, 25-30 June, 2007. 10 pages, 5 figures, and 1 table
arxiv created 2007/10/02 · openalex publication_date 2007/10/02 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Properties of effective interactions in neutron-rich matter are reflected in the medium's equation of state (EOS), which is a relationship among several state variables. Spin and isospin asymmetries play an important role in the energy balance and could alter the stability conditions of the nuclear EOS. The EOS has far-reaching consequences for numerous nuclear processes in both the terrestrial laboratories and the cosmos. Presently the EOS, especially for neutron-rich matter, is still very uncertain. Heavy-ion reactions provide a unique means to constrain the EOS, particularly the density dependence of the nuclear symmetry energy. On the other hand, microscopic, self-consistent, and parameter-free approaches are ultimately needed for understanding nuclear properties in terms of the fundamental interactions among the basic constituents of nuclear systems. In this talk, after a brief review of our recent studies on spin-polarized neutron matter, we discuss constraining the changing rate of the gravitational constant G and properties of (rapidly) rotating neutron stars by using a nuclear EOS partially constrained by the latest terrestrial nuclear laboratory data.