Binary black holes in magnetized disks of active galactic nuclei

¹ Nicolaus Copernicus Astronomical Center of the Polish Academy of Sciences, Bartycka 18, PL-00-716 Warsaw, Poland
² Department of Astronomy, Astrophysics and Space Engineering, Indian Institute of Technology Indore, Indore 453552, India
³ Gran Sasso Science Institute (GSSI), I-67100 L’Aquila, Italy
⁴ Departament d’Astronomia i Astrofísica, Universitat de València, C/ Dr Moliner 50, 46100 Burjassot (València), Spain
⁵ Department of Physics, University of Illinois at Urbana-Champaign, Urbana, IL 61801, USA
⁶ National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, Urbana, IL 61801, USA
⁷ Research Center for Astronomy and Applied Mathematics, Academy of Athens, Athens 11527, Greece
⁸ Dipartimento di Fisica, Universitá degli Studi di Torino, Via Pietro Giuria 1, I-10125 Torino, Italy
⁹ Nicolaus Copernicus Superior School, College of Astronomy and Natural Sciences, Gregorkiewicza 3, 87-100 Toruń, Poland
¹⁰ Research Centre for Computational Physics and Data Processing, Institute of Physics, Silesian University in Opava, Bezručovo nám. 13, CZ-746 01 Opava, Czech Republic

^⋆ Corresponding author: rjoshi@camk.edu.pl

Received: 9 June 2025
Accepted: 19 September 2025

Abstract

Stellar-mass binary black hole (BBH) mergers that occur within the disks of active galactic nuclei (AGN) are promising sources for gravitational waves that can be detected by the LIGO, Virgo, and KAGRA interferometers. Some of these events have also been potentially associated with transient electromagnetic flares, indicating that BBH mergers in dense environments may be promising sources of multimessenger signals. To investigate the prospects for electromagnetic emission from these systems, we studied the dynamics of accretion flows onto BBHs that are embedded in AGN disks with numerical simulations. Although recent studies have explored this scenario, they often employed simplified disk models that neglected magnetic fields. We examined how strong magnetic fields affect and regulate the accretion onto these binary systems. In this context, we conducted three-dimensional magnetohydrodynamical local shearing-box simulations of a BBH system embedded within a magnetized disk of an AGN. The dynamically important magnetic fields can drive the formation of well-collimated outflows that can penetrate the vertical extent of the AGN disk. The outflow generation is not ubiquitous, however, and strongly depends on the radial distance of the binary from the supermassive black hole (SMBH). In particular, binaries placed at a larger distance from the central SMBH show a relatively stronger transient accretion and the formation of stronger spiral shocks. Furthermore, the accretion behavior onto the binary system via individual circum-singular disks is also modulated by local AGN disk properties. Our simulations highlight the importance of the shear velocity in the amplification of the toroidal magnetic field component, which plays a crucial role in governing the outflow strength.