Hyper-neutron stars from an ab initio calculation

TL;DR

This paper presents an ab initio quantum Monte Carlo calculation of hyper-neutron matter to derive equations of state, predicting neutron star properties consistent with observations and exploring rotational effects on maximum mass.

Contribution

It introduces a novel ab initio approach to hyper-neutron matter using auxiliary field quantum Monte Carlo and Nuclear Lattice EFT, including hyperon interactions.

Findings

Maximum neutron star mass predicted as 2.17 solar masses.

Predicted radius for 1.4 solar mass neutron star is 13.10 km.

Tidal deformability for 1.4 solar mass neutron star is 597.

Abstract

The equation of state (EoS) of neutron matter plays a decisive role to understand the neutron star properties and the gravitational waves from neutron star mergers. At sufficient densities, the appearance of hyperons generally softens the EoS, leading to a reduction in the maximum mass of neutron stars well below the observed values of about 2 solar masses. Even though repulsive three-body forces are known to solve this so-called ``hyperon puzzle'', so far performing \textit{ab initio} calculations with a substantial number of hyperons for neutron star properties has remained elusive. Starting from the newly developed auxiliary field quantum Monte Carlo algorithm to simulate hyper-neutron matter (HNM) without any sign oscillations, we derive three distinct EoSs by employing the state-of-the-art Nuclear Lattice Effective Field Theory. We include $N\Lambda$, $\Lambda\Lambda$ two-body forces, $NN\Lambda$, and $N\Lambda\Lambda$ three-body forces. Consequently, we determine essential astrophysical quantities such as the neutron star mass, radius, tidal deformability, and the universal $I$-Love-$Q$ relation. The maximum mass, radius and tidal deformability of a $1.4M_\odot$ neutron star are predicted to be $2.17(1)(1)~M_\odot$, $R_{1.4M\odot}=13.10(1)(7)~$km, and $\Lambda_{1.4M_\odot}=597(5)(18)$, respectively, based on our most realistic EoS. These predictions are in good agreement with the latest astrophysical constraints derived from observations of massive neutron stars, gravitational waves, and joint mass-radius measurements. Also, for the first time in \textit{ab initio} calculations, we investigate both non-rotating and rotating neutron star configurations. The results indicate that the impact of rotational dynamics on the maximum mass is small, regardless of whether hyperons are present in the EoS or not.