2023MNRAS.518.6158J

The recent detections of binary stellar mass black hole mergers by the LIGO and Virgo Collaborations suggest that such mergers are common occurrences. Galaxy mergers further indicate that supermassive black holes in centres of galaxies also merge and are typically expected to have had at least one merger in their lifetime, possibly many. In the presence of a jet, these mergers are almost always accompanied by a change of the jet direction and a connected jet precession motion, leading to interactions of the jet with ambient matter and producing high-energy particles, and consequently high-energy gamma-rays and neutrinos. In this work, we investigate the possibility under which conditions such mergers could be the sources of the diffuse astrophysical neutrino flux measured by the IceCube Neutrino Observatory. The main free parameters in the calculation concern the frequency of the mergers and the fraction of energy that is transferred from the gravitationally released energy to neutrinos. We show that the merger rate for SMBBHs must lie between ∼10^–7 and 10^–5 Gpc^–3 yr^–1. The ratio of energy going to neutrinos during such mergers lies then between ∼10^–6 and 3 × 10^–4. For stellar mass BBH mergers, the rate needs to be ∼10-100 Gpc^–3 yr^–1 and the expected ratio of neutrino to GW energy lies in a comparable range as for SMBBHs, ∼2 × 10^–5-10^–3. These values lie in a reasonable parameter range, so that the production of neutrinos at the level of the detected neutrino flux is a realistic possibility.