Relativistic Equation of State of Nuclear Matter for Supernova and Neutron Star
H. Shen, H. Toki, K. Oyamatsu, K. Sumiyoshi
Abstract
We construct the equation of state (EOS) of nuclear matter using the relativistic mean field (RMF) theory in the wide density, temperature range with various proton fractions for the use of supernova simulation and the neutron star calculations. We first construct the EOS of homogeneous nuclear matter. We use then the Thomas-Fermi approximation to describe inhomogeneous matter, where heavy nuclei are formed together with free nucleon gas. We discuss the results on free energy, pressure and entropy in the wide range of astrophysical interest. As an example, we apply the resulting EOS on the neutron star properties by using the Oppenheimer-Volkoff equation.
Create a lesson
Related papers
Scale Invariance and Compact Star Matter
Hyun Kyu Lee, Won-Gi Paeng
Optimizing artificial neural networks for dipole strength predictions in light nuclei
Tim Egert, Weiguang Jiang, Sonia Bacca
Coupled-channel scattering from artificial confinement
Tafat Weiss Attia, Itay Horin, Betzalel Bazak
From twelve to three active qubits: Ancilla-recycled rodeo filtering for trapped neutron-proton scattering
Myeong-Hwan Mun, Jubin Park, Myung-Ki Cheoun et al.
Single-particle potentials in asymmetric nuclear matter within the LOCV framework
Zahra Ziarati, Hamidreza Moshfegh
Frontier Questions and Emerging Directions in Nuclear Science and Technology
Yu-Gang Ma