Mass ejection from neutron star mergers: different components and expected radio signals

TL;DR

This paper reviews the different components of mass ejected during neutron star mergers and predicts their distinct radio signals, emphasizing how viewing angle and external density influence detectability with current radio telescopes.

Contribution

It provides a comprehensive analysis of the various ejecta components and their expected radio signatures, including the effects of viewing angle and external medium density.

Findings

Relativistic ejecta produce early radio afterglows detectable within days.

Non-relativistic ejecta dominate radio signals at larger viewing angles after about a year.

Radio signals from ejecta are detectable with EVLA and LOFAR under certain conditions.

Abstract

In addition to producing a strong gravitational signal, a short gamma-ray burst (GRB), and a compact remnant, neutron star mergers eject significant masses at significant kinetic energies. This mass ejection takes place via dynamical mass ejection and a GRB jet but other processes have also been suggested: a shock-breakout material, a cocoon resulting from the interaction of the jet with other ejecta, and viscous and neutrino driven winds from the central remnant or the accretion disk. The different components of the ejected masses include up to a few percent of a solar mass, some of which is ejected at relativistic velocities. The interaction of these ejecta with the surrounding interstellar medium will produce a long lasting radio flare, in a similar way to GRB afterglows or to radio supernovae. The relative strength of the different signals depends strongly on the viewing angle. An observer along the jet axis or close to it will detect a strong signal at a few dozen days from the radio afterglow (or the orphan radio afterglow) produced by the highly relativistic GRB jet. For a generic observer at larger viewing angles, the dynamical ejecta, whose contribution peaks a year or so after the event, will generally dominate. Depending on the observed frequency and the external density, other components may also give rise to a significant contribution. We also compare these estimates with the radio signature of the short GRB 130603B. The radio flare from the dynamical ejecta might be detectable with the EVLA and the LOFAR for the higher range of external densities $n\gtrsim 0.5{\rm cm^{-3}}$.