Gravitational and magnetosonic waves in gamma-ray bursts

TL;DR

This paper explores how gravitational waves from merging neutron star binaries can transfer energy to magnetohydrodynamic waves in the surrounding plasma wind, using relativistic MHD equations and linear analysis.

Contribution

It introduces a relativistic MHD framework to analyze GW-induced wave growth in magnetized plasma around neutron star mergers.

Findings

Fast magneto-acoustic waves grow proportionally to GW amplitude and frequency.

The background magnetic field influences the wave growth.

Relativistic MHD equations are derived for this scenario.

Abstract

One of the possible sources of gamma-ray bursts are merging, compact neutronstar binaries. More than 90% of the binding energy of such a binary is released in the form of gravitational waves (GWs) in the last few seconds of the spiral-in phase before the formation of a black hole. In this article we investigate whether a fraction of this GW-energy is transferred to magnetohydrodynamic waves in the magnetized plasma wind around the binary. Using the 3+1 orthonormal tedrad formalism, we study the propagation of a monochromatic, plane fronted, linearly polarized GW perpendicular to the ambient magnetic field in an ultra-relativistic wind, first in the comoving and then in the observer frame. A closed set of general relativistic magnetohydrodynamic equations is derived in the form of conservation laws for electric charge, matter energy, momentum and magnetic energy densities. We linearize these equations under the action of a monochromatic GW, which acts as a driver and find that fast magneto-acoustic waves grow, with amplitudes proportional to the GW amplitude and frequency and the strength of the background magnetic field.