# Searching for hypermassive neutron stars with short gamma-ray bursts

## TL;DR

This paper explores the potential for detecting hypermassive neutron star oscillations through short gamma-ray burst observations, which could reveal details about neutron star physics and the emission mechanisms of these bursts.

## Contribution

It discusses the prospects of identifying HMNS oscillations in SGRB data and their implications for understanding neutron star equations of state and burst emission mechanisms.

## Key findings

- HMNS oscillations emit high-frequency GWs difficult to detect directly.
- Detection of oscillations via SGRB modulation could provide new insights.
- Understanding these signals informs neutron star physics and gamma-ray burst models.

## Abstract

Neutron star mergers can form a hypermassive neutron star (HMNS) remnant, which may be the engine of a short gamma ray burst (SGRB) before it collapses to a black hole, possibly several hundred milliseconds after the merger. During the lifetime of a HMNS, numerical relativity simulations indicate that it will undergo strong oscillations and emit GWs with frequencies of a few kilohertz, which are unfortunately too high for detection to be probable with Advanced LIGO. Here we discuss the current and future prospects for detecting these oscillations as modulation of the SGRB. The understanding of the physical mechanism responsible for the HMNS oscillations will provide information on the equation of state of the hot HMNS, and the observation of these frequencies in the SGRB data would give us insight into the emission mechanism of the SGRB.