Impacts of anomaly on nuclear and neutron star equation of state based on a parity doublet model

TL;DR

This paper investigates how the $U(1)_A$ anomaly influences nuclear and neutron star equations of state using a parity doublet model, revealing that the anomaly softens EOSs and affects neutron star properties.

Contribution

It introduces the impact of the $U(1)_A$ anomaly via the KMT interaction into the parity doublet model and updates the neutron star EOSs accordingly.

Findings

The $U(1)_A$ anomaly increases meson masses and enhances chiral symmetry breaking.

Anomaly effects soften the EOSs, reducing neutron star radii.

The chiral invariant mass $m_0$ is constrained to 400-700 MeV, smaller than previous estimates.

Abstract

We examine the role of the $U(1)_A$ anomaly in a parity doublet model of nucleons which include the chiral variant and invariant masses. Our model expresses the $U(1)_A$ anomaly by the Kobayashi-Maskawa-'t\,Hooft (KMT) interaction in the mesonic sector. After examining the roles of the KMT term in vacuum, we discuss its impacts on nuclear equations of state (EOS). The $U(1)_A$ anomaly increases the masses of the $\eta'$ and $\sigma$ mesons and enhances the chiral symmetry breaking. The $U(1)_A$ anomaly enlarges the energy difference between chiral symmetric and symmetry broken vacuum; in turn, the chiral restoration at high density adds a larger energy density (often referred as a bag constant) to EOSs than in the case without the anomaly, leading to softer EOSs. Including these $U(1)_A$ effects, we update the previously constructed unified equations of state that interpolate the nucleonic EOS at $n_B \le 2n_0$ ($n_{0} = 0.16\, \rm{fm^{-3}}$: nuclear saturation density) and quark EOS at $n_B \ge 5n_0$. The unified EOS is confronted with the observational constraints on the masses and radii of neutron stars. The softening of EOSs associated with the $U(1)$ anomaly reduces the overall radii, relaxing the previous constraint on the chiral invariant mass $m_0$. Including the attractive nonlinear $\rho$-$\omega$ coupling to improved estimates for the slope parameter in the symmetry energy, our new estimate is $400\,{\rm MeV} \leq m_0 \leq 700\,{\rm MeV}$, with $m_0$ smaller than our previous estimate by $\sim 200$ MeV.