Evolution and instabilities of disks harboring super massive black holes

TL;DR

This study uses numerical simulations to analyze how supermassive black holes influence the formation and stability of stellar bars in galactic disks, revealing a mild impact on bar ellipticity and growth dynamics.

Contribution

It provides new insights into the role of central black holes in bar formation and evolution through detailed N-body-SPH simulations in isolated and cosmological scenarios.

Findings

Black holes have a mild effect on bar ellipticity.

Bars persist for 10 Gyrs regardless of black hole presence.

Black hole growth depends on initial mass and feedback efficiency.

Abstract

The bar formation is still an open problem in modern astrophysics. In this paper we present numerical simulation performed with the aim of analyzing the growth of the bar instability inside stellar-gaseous disks, where the star formation is triggered, and a central black hole is present. The aim of this paper is to point out the impact of such a central massive black hole on the growth of the bar. We use N-body-SPH simulations of the same isolated disk-to-halo mass systems harboring black holes with different initial masses and different energy feedback on the surrounding gas. We compare the results of these simulations with the one of the same disk without black hole in its center. We make the same comparison (disk with and without black hole) for a stellar disk in a fully cosmological scenario. A stellar bar, lasting 10 Gyrs, is present in all our simulations. The central black hole mass has in general a mild effect on the ellipticity of the bar but it is never able to destroy it. The black holes grow in different way according their initial mass and their feedback efficiency, the final values of the velocity dispersions and of the black hole masses are near to the phenomenological constraints.