Nuclear equation of state at high density and the properties of neutron stars

Abstract

We discuss the relativistic nuclear equation of state (EOS) using a relativistic transport model in heavy-ion collisions. From the baryon flow for $Au+Au$ systems at SIS to AGS energies and above we find that the strength of the vector potential has to be reduced moderately at high density or at high relative momenta to describe the flow data at 1-10 A GeV. We use the same dynamical model to calculate the nuclear EOS and then employ this to calculate the gross structure of the neutron star considering the core to be composed of neutrons with an admixture of protons, electrons, muons, sigmas and lambdas at zero temperature. We then discuss these gross properties of neutron stars such as maximum mass and radius in contrast to the observational values.

17 pages, 5 figures, to be published in Phy. Rev. C

References in corpus (6)

• Elliptic Flow: Transition from out-of-plane to in-plane Emission in Au + Au Collisions
• Sideward Flow in Au + Au Collisions Between 2A GeV and 8A GeV
• Phase Transitions in Neutron Stars and Maximum Masses
• Baryon flow from SIS to AGS energies
• A Schematic Model for $\rho$-$a_1$ Mixing at Finite Density and In-Medium Effective Lagrangian
• Renormalization Group Analysis of ρ-Meson Properties at Finite Density

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• Maximum mass of neutron stars with a quark core
• Complete relativistic equation of state for neutron stars
• Hot Nuclear Matter in Asymmetry Chiral Sigma Model
• Interplay between kaon condensation and hyperons in highly dense matter
• Kaon Condensation and Lambda-Nucleon Loop in the Relativistic Mean-Field Approach
• Radial Modes of Neutron Stars with a Quark Core
• Kaonic modes in hyperonic matter and p-wave kaon condensation
• Nuclear Matter and Finite Nuclei in the Effective Chiral Model
• Thermal properties of hot and dense medium in interacting hadron resonance gas model
• Relativistic Neutron Stars: Rheological Type Extensions of the Equations of State