Neutron Star Mergers in AGN Accretion Disks: Cocoon and Ejecta Shock Breakouts

TL;DR

This paper predicts observable X-ray and UV shock breakout signals from neutron star mergers in AGN disks, highlighting potential multi-messenger signatures for identifying such events.

Contribution

It introduces a model where jet choked in AGN disks produces detectable shock breakout transients, linking gravitational wave sources to electromagnetic signals in this environment.

Findings

Bright X-ray shock breakout peaking at 0.15 days

UV flare peaking at 0.5 days from ejecta breakout

Detectability by current and future transient surveys

Abstract

Neutron star mergers are believed to occur in accretion disks around supermassive black holes. Here we show that a putative jet launched from the merger of a binary neutron star (BNS) or a neutron star--black hole (NSBH) merger occurring at the migration trap in an active galactic nucleus (AGN) disk would be choked. The jet energy is deposited within the disk materials to power a hot cocoon. The cocoon is energetic enough to break out from the AGN disk and produce a bright X-ray shock breakout transient peaking at $\sim0.15\,{\rm d}$ after the merger. The peak luminosity is estimated as $\sim 10^{46}\,{\rm erg}\,{\rm s}^{-1}$, which can be discovered by Einstein Probe from $z\lesssim 0.5$. Later on, the non-relativistic ejecta launched from the merger would break out the disk, powering an X-ray/UV flare peaking at $\sim 0.5\,{\rm d}$ after the merger. This second shock breakout signal may be detected by UV transient searches. The cocoon cooling emission and kilonova emission are outshone by the disk emission and difficult to be detected. Future joint observations of gravitational waves from BNS/NSBH mergers and associated two shock breakout signatures can provide a strong support for the compact binary coalescence formation channel in AGN disks.