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The complex evolution of supermassive black holes in cosmological simulations

Published online by Cambridge University Press:  20 January 2023

Peter H. Johansson Open the ORCID record for Peter H. Johansson [Opens in a new window] ,
Matias Mannerkoski ,
Antti Rantala ,
Shihong Liao ,
Alexander Rawlings ,
Dimitrios Irodotou  and
Francesco Rizzuto
Peter H. Johansson
Affiliation:
Department of Physics, Gustaf Hällströmin katu 2, FI-00014, University of Helsinki, Finland email: [email protected]
Matias Mannerkoski
Affiliation:
Department of Physics, Gustaf Hällströmin katu 2, FI-00014, University of Helsinki, Finland email: [email protected]
Antti Rantala
Affiliation:
Max-Planck Institut für Astrophysik, Karl-Schwarzschild-Str 1, D-85748, Garching, Germany
Shihong Liao
Affiliation:
Department of Physics, Gustaf Hällströmin katu 2, FI-00014, University of Helsinki, Finland email: [email protected]
Alexander Rawlings
Affiliation:
Department of Physics, Gustaf Hällströmin katu 2, FI-00014, University of Helsinki, Finland email: [email protected]
Dimitrios Irodotou
Affiliation:
Department of Physics, Gustaf Hällströmin katu 2, FI-00014, University of Helsinki, Finland email: [email protected]
Francesco Rizzuto
Affiliation:
Department of Physics, Gustaf Hällströmin katu 2, FI-00014, University of Helsinki, Finland email: [email protected]
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Abstract

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We present here self-consistent zoom-in simulations of massive galaxies forming in a full cosmological setting. The simulations are run with an updated version of the KETJU code, which is able to resolve the gravitational dynamics of their supermassive black holes, while simultaneously modelling the large-scale astrophysical processes in the surrounding galaxies, such as gas cooling, star formation and stellar and AGN feedback. The KETJU code is able to accurately model the complex behaviour of multiple SMBHs, including dynamical friction, stellar scattering and gravitational wave emission, and also to resolve Lidov–Kozai oscillations that naturally occur in hierarchical triplet SMBH systems. In general most of the SMBH binaries form at moderately high eccentricities, with typical values in the range of , meaning that the circular binary models that are commonly used in the literature are insufficient for capturing the typical binary evolution.

Keywords

galaxies: supermassive black holesgalaxies: formationgalaxies: elliptical and lenticularmethods: numerical
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 16 , Symposium S362: The Predictive Power of Computational Astrophysics as a Discovery Tool , June 2020 , pp. 33 - 38
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

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