The multi-messenger picture of compact object encounters: binary mergers versus dynamical collisions

TL;DR

This paper compares the multi-messenger signals of neutron star mergers and dynamical collisions, analyzing their gravitational waves, neutrinos, ejecta, and electromagnetic counterparts to understand their astrophysical implications.

Contribution

It provides a detailed comparison of gravitational, neutrino, and electromagnetic signatures of binary mergers versus dynamical collisions, highlighting differences in ejecta and observational prospects.

Findings

NSNS mergers eject over 1% solar mass of neutron-rich material, contributing to r-process nucleosynthesis.

NSBH collisions eject large amounts of matter (~0.15 solar masses), constraining their occurrence rates.

Electromagnetic transients like macronovae peak within days, with luminosities up to 7 times higher in collisions.

Abstract

We explore the multi-messenger signatures of encounters between two neutron stars and between a neutron star and a stellar-mass black hole. We focus on the differences between gravitational wave driven binary mergers and dynamical collisions that occur, for example, in globular clusters. For both types of encounters we compare the gravitational wave and neutrino emission properties. We also calculate fallback rates and analyze the properties of the dynamically ejected matter. Last but not least we address the electromagnetic transients that accompany each type of encounter. The canonical nsns merger case ejects more than 1% of a solar mass of extremely neutron-rich ($Y_e\sim 0.03$) material, an amount that is consistent with double neutron star mergers being a major source of r-process in the galaxy. nsbh collisions eject very large amounts of matter ($\sim 0.15$ \msun) which seriously constrains their admissible occurrence rates. The compact object collision rate must therefore be less, likely much less, than 10% of the nsns merger rate. The radioactively decaying ejecta produce optical-UV "macronova" which, for the canonical merger case, peak after $\sim 0.4$ days with a luminosity of $\sim 10^{42}$ erg/s. nsns (nsbh) collisions reach up to 3 (7) times larger peak luminosities. The dynamic ejecta deposit a kinetic energy comparable to a supernova in the ambient medium. The canonical merger case releases approximately $2 \times 10^{50}$ erg, the most extreme (but likely rare) cases deposit kinetic energies of up to $10^{52}$ erg. The deceleration of this mildly relativistic material by the ambient medium produces long lasting radio flares. A canonical ns$^2$ merger at the detection horizon of advanced LIGO/Virgo produces a radio flare that peaks on a time scale of one year with a flux of $\sim$0.1 mJy at 1.4 GHz.