Nuclear pasta and symmetry energy in the relativistic point-coupling model

TL;DR

This paper investigates how nuclear symmetry energy influences the formation and properties of nuclear pasta structures in neutron-star matter using three-dimensional relativistic mean-field calculations.

Contribution

It introduces a coupling between isoscalar and isovector interactions in a relativistic point-coupling model to study pasta phases and their dependence on symmetry energy.

Findings

Pasta structures are strongly affected by symmetry energy and its slope.

Various pasta shapes, including intermediate structures, are observed in cold stellar matter.

Nonspherical shapes are unlikely in neutron-star crusts due to low proton fractions.

Abstract

Nonuniform structure of low-density nuclear matter, known as nuclear pasta, is expected to appear not only in the inner crust of neutron stars but also in core-collapse supernova explosions and neutron-star mergers. We perform fully three-dimensional calculations of inhomogeneous nuclear matter and neutron-star matter in the low-density region using the Thomas-Fermi approximation. The nuclear interaction is described in the relativistic mean-field approach with the point-coupling interaction, where the meson exchange in each channel is replaced by the contact interaction between nucleons. We investigate the influence of nuclear symmetry energy and its density dependence on pasta structures by introducing a coupling term between the isoscalar-vector and isovector-vector interactions. It is found that the properties of pasta phases in the neutron-rich matter are strongly dependent on the symmetry energy and its slope. In addition to typical shapes like droplets, rods, slabs, tubes, and bubbles, some intermediate pasta structures are also observed in cold stellar matter with a relatively large proton fraction. We find that nonspherical shapes are unlikely to be formed in neutron-star crusts, since the proton fraction obtained in $\beta$ equilibrium is rather small. The inner crust properties may lead to a visible difference in the neutron-star radius.