# Supernovae in massive binaries and compact object mergers near supermassive black holes

## TL;DR

This paper models the evolution of supernovae in massive binaries near supermassive black holes, showing how these systems can produce gravitational wave mergers with high eccentricities, but at lower rates than observed.

## Contribution

It introduces high-precision N-body simulations including post-Newtonian effects to study supernovae in dense galactic nuclei and their role in compact binary mergers near SMBHs.

## Key findings

- Larger natal kicks produce more compact, closer mergers.
- Most mergers enter the LIGO band with high eccentricities.
- Calculated merger rates are below current LIGO-Virgo observations.

## Abstract

Nuclear star clusters that surround supermassive black holes (SMBHs) in galactic nuclei are among the densest systems in the Universe, harbouring millions of stars and compact objects (COs). Within a few parsecs from the SMBH, stars can form binaries. In this paper, we model the supernova (SN) process of massive binaries that are born in proximity of the SMBH and that produce CO binaries. These binaries can later merge via emission of gravitational waves as a consequence of the Lidov-Kozai mechanism. We study the dynamical evolution of these systems by means of high-precision $N$-body simulations, including post-Newtonian (PN) terms up to 2.5PN order. We adopt different prescriptions for the natal velocity kicks imparted during the SN processes and find that larger kicks lead to more compact binaries that merge closer to the SMBH. We also conclude that most of the mergers enter the LIGO band with very high eccentricities. Finally, we compute a merger rate of $0.05$--$0.07\ \mathrm{Gpc}^{-3} \mathrm{yr}^{-1}$, $0.04$--$2\times 10^{-3}\ \mathrm{Gpc}^{-3} \mathrm{yr}^{-1}$, $9.6\times 10^{-6}$--$2.7\times 10^{-3}\ \mathrm{Gpc}^{-3} \mathrm{yr}^{-1}$ for BH-BH, BH-NS, NS-NS, respectively, smaller than the actual LIGO-Virgo observed rate.