Merging neutron star binaries: equation of state and electrodynamics

TL;DR

This paper reviews the hydrodynamical and electrodynamical processes in merging neutron star binaries, emphasizing how gravitational wave and electromagnetic observations can constrain the neutron star equation of state during the pre-merger phase.

Contribution

It provides a comprehensive review of the physical processes in neutron star mergers, highlighting the potential for multi-messenger observations to inform nuclear physics.

Findings

GW observations can constrain the neutron star equation of state.

Electromagnetic signals from mergers can complement gravitational wave data.

Hydrodynamical and electrodynamical processes influence the merger dynamics.

Abstract

Merging neutron star (NS) binaries may be detected by ground-based gravitational wave (GW) interferometers (e.g. LIGO/VIRGO) within this decade and may also generate electromagnetic radiation detectable by wide-field, fast imaging telescopes that are coming online. The GWs can provide new constraint on the NS equation of state (including mass-radius relation and the related nuclear symmetry energy through resonant g-modes). This paper reviews various hydrodynamical (including equilibrium and dynamical/resonant tides) and electrodynamical processes in coalescing NS binaries, with focus on the pre-merger phase.