Simulating Binary Black Holes embedded in AGN disks

by Raj Kishor Joshi (Nicolaus Copernicus Astronomical Center of the Polish Academy of Sciences)

Friday 14 Mar 2025, 14:00 → 16:00 Europe/Berlin

Abbeanum/1-102 - Seminarraum (TPI, FSU Jena)

The gravitational signals detected by LIGO/Virgo/KAGRA runs are dominated by those from
stellar-mass binary black hole mergers. Currently, the astrophysical environments where such
BBHs form are not known very well, and several channels have been proposed as plausible
origins for forming these merging systems. Gravitational wave observations play a crucial role in
determining the masses of merging compact objects. However, to gain a deeper understanding
of the environments in which these mergers occur, electromagnetic signatures are equally
important. Unlike mergers involving a neutron star, binary black hole mergers present a unique
challenge for electromagnetic observations. Since isolated black holes do not emit any
electromagnetic radiation, their detection is only possible if they occur in a gas-rich environment,
where surrounding matter can produce observable emissions. Active galactic nucleus disks offer
such a favorable setting. We simulate the equal-mass binary black holes embedded
in the Keplerian disk of an AGN. Using magnetohydrodynamical simulations, we explore various
scenarios that may offer interesting observational prospects for electromagnetic counterparts.