Hypernuclear Physics for Neutron Stars

TL;DR

This paper reviews how hypernuclear physics influences neutron star properties, including composition, equation of state, cooling, and gravitational wave emissions, highlighting the importance of hyperon interactions in dense matter.

Contribution

It elucidates the impact of hypernuclear potentials and interactions on neutron star structure, cooling, and gravitational wave signals, integrating hypernuclear physics into neutron star modeling.

Findings

Hyperon potentials determine neutron star composition.

Three-body interactions affect the star's maximum mass.

Hyperon pairing suppresses neutron star cooling.

Abstract

The role of hypernuclear physics for the physics of neutron stars is delineated. Hypernuclear potentials in dense matter control the hyperon composition of dense neutron star matter. The three-body interactions of nucleons and hyperons determine the stiffness of the neutron star equation of state and thereby the maximum neutron star mass. Two-body hyperon-nucleon and hyperon-hyperon interactions give rise to hyperon pairing which exponentially suppresses cooling of neutron stars via the direct hyperon URCA processes. Non-mesonic weak reactions with hyperons in dense neutron star matter govern the gravitational wave emissions due to the r-mode instability of rotating neutron stars.