# Neutron star crusts from mean field models constrained by chiral effective field theory

## TL;DR

This paper models neutron star crusts using Skyrme mean field models constrained by chiral effective field theory, analyzing nuclear pasta phases and the crust-core boundary to improve understanding of neutron star structure.

## Contribution

It introduces new Skyrme mean field models constrained by chiral EFT and ground-state energies, providing detailed analysis of nuclear pasta phases and crust properties.

## Key findings

- Wigner-Seitz cell size varies with model parameters
- Nuclear pasta phases depend on density and geometry
- Thermodynamic instability method validates energy-based solutions

## Abstract

We investigate the structure of neutron star crusts, including the crust-core boundary, based on new Skyrme mean field models constrained by the bulk-matter equation of state from chiral effective field theory and the ground-state energies of doubly-magic nuclei. Nuclear pasta phases are studied using both the liquid drop model as well as the Thomas-Fermi approximation. We compare the energy per nucleon for each geometry (spherical nuclei, cylindrical nuclei, nuclear slabs, cylindrical holes, and spherical holes) to obtain the ground state phase as a function of density. We find that the size of the Wigner-Seitz cell depends strongly on the model parameters, especially the coefficients of the density gradient interaction terms. We employ also the thermodynamic instability method to check the validity of the numerical solutions based on energy comparisons.