Nuclear constraints on the core-crust transition density and pressure of neutron stars

TL;DR

This paper constrains the core-crust transition density and pressure of neutron stars using recent nuclear matter equations of state, revealing significant differences from previous approximations and improving neutron star mass-radius relations.

Contribution

It provides new constraints on transition density and pressure using recent experimental data, highlighting the impact of approximation methods on these estimates.

Findings

Transition density: 0.040-0.065 fm^{-3}

Transition pressure: 0.01-0.26 MeV/fm^{3}

Improved mass-radius relation for neutron stars

Abstract

Using the equation of state of asymmetric nuclear matter that has been recently constrained by the isospin diffusion data from intermediate-energy heavy ion collisions, we have studied the transition density and pressure at the inner edge of neutron star crusts, and they are found to be 0.040 fm^{-3} <= \rho_{t}<= 0.065 fm^{-3} and 0.01 MeV/fm^{3} <= P_{t} <= 0.26 MeV/fm^{3}, respectively, in both the dynamical and thermodynamical approaches. We have further found that the widely used parabolic approximation to the equation of state of asymmetric nuclear matter gives significantly higher values of core-crust transition density and pressure, especially for stiff symmetry energies. With these newly determined transition density and pressure, we have obtained an improved relation between the mass and radius of neutron stars based on the observed minimum crustal fraction of the total moment of inertia for Vela pulsar.