Tidal deformability of neutron and hyperon star with relativistic mean field equations of state

TL;DR

This paper investigates how the internal composition of neutron and hyperon stars affects their tidal deformability, which influences gravitational wave signals during binary mergers, using relativistic mean field equations of state.

Contribution

It provides a systematic analysis of tidal deformability for neutron and hyperon stars based on RMF equations of state, highlighting its impact on gravitational wave signatures.

Findings

Tidal deformability varies with star composition and EOS.

Deformability has a small correction but a clear gravitational wave signature.

Potential for measurement with advanced LIGO during binary inspiral.

Abstract

We systematically study the tidal deformability for neutron and hyperon stars using relativistic mean field (RMF) equations of state (EOSs). The tidal effect plays an important role during the early part of the evolution of compact binaries. Although, the deformability associated with the EOSs has a small correction, it gives a clean gravitational wave signature in binary inspiral. These are characterized by various love numbers kl (l=2, 3, 4), that depend on the EOS of a star for a given mass and radius. The tidal effect of star could be efficiently measured through advanced LIGO detector from the final stages of inspiraling binary neutron star (BNS) merger.