Estimates of the early EM emission from compact binary mergers

TL;DR

This paper models early electromagnetic emissions from compact binary mergers involving neutron stars or black holes, linking luminosity and timescales to gravitational wave parameters to aid in identifying merger types.

Contribution

It provides estimates of early EM emission luminosities and timescales based on chirp mass, especially in the mass gap range, to distinguish merger types from gravitational wave data.

Findings

Electromagnetic transients can differentiate merger types within specific chirp mass ranges.

For GRB GBM-190816, the analysis suggests a high effective spin and a heavier component mass.

The study connects gravitational wave parameters with early EM signals to improve merger characterization.

Abstract

Compact binary mergers that involve at least one neutron star, either binary neutron star or black hole--neutron star coalescences, are thought to be the potential sources of electromagnetic emission due to the material ejected during the merger or those left outside the central object after the merger. Since the intensity of these electromagnetic transients decay rapidly with time, one should pay more attention to early emissions from such events, which are useful in revealing the nature of these mergers. In this work, we study the early emission of kilonovae, short $\gamma$-ray bursts and cocoons that could be produced in those mergers. We estimate their luminosities and time scales as functions of the chirp mass which is the most readily constrained parameter from the gravitational wave detections of these events. We focus on the range of chirp mass as $1.3M_{\odot} -2.7M_{\odot}$ which is compatible with one of the merging component being a so-called `mass gap' black hole. We show that the electromagnetic observation of these transients could be used to distinguish the types of the mergers when the detected chirp mass falls in the range of $1.5M_{\odot}-1.7M_{\odot}$. Applying our analysis to the sub-threshold GRB GBM-190816, we found that for this particular event the effective spin should be larger than 0.6 and the mass of the heavier object might be larger than 5.5$M_{\odot}$ for the SFHo equation of state.