# N-Body Simulations of Gas-free Disc Galaxies with SMBH Seed in Binary Systems

## TL;DR

This study uses N-body simulations to analyze the evolution of supermassive black hole seeds during galaxy mergers, revealing significant SMBH growth and the impact of tidal effects on galaxy morphology.

## Contribution

It introduces detailed N-body simulations of gas-free disc galaxy mergers with initial SMBH seeds, exploring SMBH growth and galaxy morphology changes over cosmic time.

## Key findings

- SMBHs can grow by factors of 6 to 64 during mergers.
- Merger remnants can be warped or thicker discs.
- Tidal effects influence SMBH evolution and galaxy structure.

## Abstract

We have shown the outcome of N-body simulations of the interactions of two disc galaxies without gas with the same mass. Both disc galaxies have halos of dark matter, central bulges and initial supermassive black hole (SMBH) seeds at their centers. The purpose of this work is to study the mass and dynamical evolution of the initial SMBH seed during a Hubble cosmological time. It is a complementation of our previous paper with different initial orbit conditions and by introducing the SMBH seed in the initial galaxy. The disc of the secondary galaxy has coplanar or polar orientation in relation to the disc of the primary galaxy and their initial orbit are eccentric and prograde. The primary and secondary galaxies have mass and size of Milky Way with an initial SMBH seed. We have found that the merger of the primary and secondary discs can result in a final normal disc or a final warped disc. After the fusion of discs, the final one is thicker and larger than the initial disc. The tidal effects are very important, modifying the evolution of the SMBH in the primary and secondary galaxy differently. The mass of the SMBH of the primary galaxy have increased by a factor ranging from 52 to 64 times the initial seed mass, depending on the experiment. However, the mass of the SMBH of the secondary galaxy have increased by a factor ranging from 6 to 33 times the initial SMBH seed mass, depending also on the experiment. Most of the accreted particles have come from the bulge and from the halo, depleting their particles. This could explain why the observations show that the SMBH with masses of approximately $10^6 M_\odot$ are found in many bulgeless galaxies. Only a small number of the accreted particles has come from the disc. In some cases of final merging stage of the two galaxies, the final SMBH of the secondary galaxy was {ejected out of the galaxy}.