Impact of the Scalar Isovector $\delta$-meson on the description of nuclear matter and neutron star properties

TL;DR

This paper investigates how including the scalar isovector δ-meson in a relativistic mean-field model influences nuclear matter and neutron star properties, notably affecting the symmetry energy, radius, and tidal deformability.

Contribution

It introduces a Bayesian inference method to determine model parameters and demonstrates the δ-meson's significant impact on symmetry energy and neutron star observables.

Findings

δ-meson inclusion affects neutron star radius and deformability

It allows for a wider range of symmetry energy parameters

The maximum neutron star mass is only slightly affected

Abstract

The implications of including the scalar isovector $\delta$-meson in a relativistic mean-field description of nuclear matter are discussed. A Bayesian inference approach is used to determine the parameters that define the isovector properties of the model. The properties of nuclear matter and neutron stars are discussed. The inclusion of the $\delta$-meson has only a small effect on the maximum mass of the neutron star (NS) and on the speed of sound in its interior, but it has a strong effect on the radius and the tidal deformability of low and medium mass stars. This is mainly due to the effect of the $\delta$-meson on the symmetry energy and its slope and curvature at saturation, increasing the range of possible values of these three properties, and in particular allowing positive values of the symmetry energy curvature. Due to the effect of the $\delta$-meson on the symmetry energy, the proton content of the star is also strongly affected. The inclusion of the $\delta$-meson in the relativistic mean-field description of nuclear matter extends the phase space spanned by the model, allowing for a more flexible density dependence of the symmetry energy compatible with experimental, observational, and ab initio constraints.