Constraining the EOS of neutron-rich nuclear matter and properties of neutron stars with heavy-ion reactions

TL;DR

This paper reviews how heavy-ion collision experiments, especially with radioactive beams, help constrain the nuclear symmetry energy, impacting our understanding of neutron star properties and related astrophysical phenomena.

Contribution

It discusses recent advancements in constraining the symmetry energy at various densities using transport models and analyzes their astrophysical implications.

Findings

Constraints on symmetry energy from isospin diffusion.

Constraints from $ ext{pi}^-/ ext{pi}^+$ ratios.

Implications for neutron star crusts and gravitational waves.

Abstract

Heavy-ion reactions especially those induced by radioactive beams provide useful information about the density dependence of the nuclear symmetry energy, thus the Equation of State of neutron-rich nuclear matter, relevant for many astrophysical studies. The latest developments in constraining the symmetry energy at both sub- and supra-saturation densities from analyses of the isopsin diffusion and the $\pi^-/\pi^+$ ratio in heavy-ion collisions using the IBUU04 transport model are discussed. Astrophysical ramifications of the partially constrained symmetry energy on properties of neutron star crusts, gravitational waves emitted by deformed pulsars and the w-mode oscillations of neutron stars are presented briefly.